FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Thompson, FC AF Thompson, FC TI The name of the type species of Simulium (Diptera : Simuliidae): An historical footnote SO ENTOMOLOGICAL NEWS LA English DT Article AB The proper original description of the type-species of the genus Simulium, S. colombaschense (Scopoli), is identified and the current spelling of the species name is confirmed. C1 Smithsonian Inst, Systemat Entomol Lab, USDA, Washington, DC 20560 USA. RP Thompson, FC (reprint author), Smithsonian Inst, Systemat Entomol Lab, USDA, Washington, DC 20560 USA. NR 14 TC 1 Z9 1 U1 0 U2 0 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0013-872X J9 ENTOMOL NEWS JI Entomol. News PD MAR-APR PY 2001 VL 112 IS 2 BP 125 EP 129 PG 5 WC Entomology SC Entomology GA 438XP UT WOS:000169079800011 ER PT J AU Sonneborn, DA AF Sonneborn, DA TI Harmonic experience SO ETHNOMUSICOLOGY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Sonneborn, DA (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC ETHNOMUSICOLOGY INC PI BLOOMINGTON PA MORRISON HALL, ROOM 005 INDIANA UNIVERSITY, BLOOMINGTON, IN 47405 USA SN 0014-1836 J9 ETHNOMUSICOLOGY JI Ethnomusicology PD SPR-SUM PY 2001 VL 45 IS 2 BP 367 EP 369 DI 10.2307/852685 PG 3 WC Music SC Music GA 430KG UT WOS:000168572600014 ER PT J AU Muss, A Robertson, DR Stepien, CA Wirtz, P Bowen, BW AF Muss, A Robertson, DR Stepien, CA Wirtz, P Bowen, BW TI Phylogeography of Ophioblennius: The role of ocean currents and geography in reef fish evolution SO EVOLUTION LA English DT Article DE biogeography; cytochrome b; dispersal; mitochondrial DNA; ocean currents; population structure; reef fishes ID ATLANTIC-OCEAN; POPULATION HISTORIES; MITOCHONDRIAL-DNA; LATE MIOCENE; GENE FLOW; PACIFIC; PANAMA; BIOGEOGRAPHY; GULF; CIRCULATION AB Many tropical reef fishes are divided into Atlantic and East Pacific taxa, placing similar species in two very different biogeographic regimes. The tropical Atlantic is a closed ocean basin with relatively stable currents, whereas the East Pacific is an open basin with unstable oceanic circulation. To assess how evolutionary processes are influenced by these differences in oceanography and geography, we analyze a 630-bp region of mitochondrial cytochrome b from 171 individuals in the blenniid genus Ophioblennius. Our results demonstrate deep genetic structuring in the Atlantic species, O. atlanticus, corresponding to recognized biogeographic provinces, with divergences of d = 5.2-12.7% among the Caribbean, Brazilian, St. Helena/Ascension Island, Gulf of Guinea, and Azores/Cape Verde regions. The Atlantic phylogeny is consistent with Pliocene dispersal from the western to eastern Atlantic, and the depth of these separations (along with prior morphological comparisons) may indicate previously unrecognized species. The eastern Pacific species, O. steindachneri. is characterized by markedly less structure than O. atlanticus, with shallow mitochondrial DNA lineages (d(max) = 2.7%) and haplotype frequency shifts between locations in the Sea of Cortez, Pacific Panama, Clipperton Island, and the: Galapagos Islands. No concordance between generic structure and biogeographic provinces was found for O. steindachneri. We attribute the phylogeographic pattern in O. atlanticus to dispersal during the reorganization of Atlantic circulation patterns that accompanied the shoaling of the Isthmus of Panama. The low degree of structure in the eastern Pacific is probably due to unstable circulation and linkage to the larger Pacific Ocean basin. The contrast in genetic signatures between Atlantic and eastern Pacific blennies demonstrates how differences in geology and oceanography have influenced evolutionary radiations within each region. C1 Univ Florida, Dept Fisheries & Aquat Sci, Gainesville, FL 32653 USA. STRI, Smithsonian Inst, Washington, DC 20560 USA. Cleveland State Univ, Ctr Environm Sci Technol & Policy, Cleveland, OH 44114 USA. Dept Oceanog & Pescas, P-9901 Horta, Azores, Portugal. RP Univ Florida, Dept Fisheries & Aquat Sci, Gainesville, FL 32653 USA. EM bowen@gnv.ifas.ufl.edu RI Stepien, Carol/A-7898-2011 NR 79 TC 157 Z9 165 U1 5 U2 39 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD MAR PY 2001 VL 55 IS 3 BP 561 EP 572 DI 10.1554/0014-3820(2001)055[0561:POOTRO]2.0.CO;2 PG 12 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 422TF UT WOS:000168134800011 PM 11327163 ER PT J AU Brauman, A Dore, J Eggleton, P Bignell, D Breznak, JA Kane, MD AF Brauman, A Dore, J Eggleton, P Bignell, D Breznak, JA Kane, MD TI Molecular phylogenetic profiling of prokaryotic communities in guts of termites with different feeding habits SO FEMS MICROBIOLOGY ECOLOGY LA English DT Article DE termite gut; gastrointestinal tract; rRNA; oligonucleolide probe; methanogen ID TARGETED OLIGONUCLEOTIDE PROBES; H-2/CO-2 ACETOGENIC BACTERIUM; RIBOSOMAL-RNA; SP-NOV; RETICULITERMES-SPERATUS; SYMBIOTIC METHANOGENS; HYBRIDIZATION PROBES; POPULATIONS; MICROFLORA; DIVERSITY AB Termites are an important group of terrestrial insects that harbor an abundant gut microbiota, many of which contribute to digestion, termite nutrition and gas (CH4, CO2 and H-2) emission. With 2200 described species, termites also provide a good model to study relationships between host diet and gut microbial community structure and function. We examined the relationship between diet and gut prokaryotic community profiles in 24 taxonomically and nutritionally diverse species of termites by using nucleic acid probes targeting 16S-like ribosomal RNAs. The relative abundance of domain-specific 16S-like rRNAs recovered from gut extracts Varied considerably (ranges: Archaea (0-3%); Bacteria (15-118%)). Although Bacteria were always detectable and the most abundant, differences in domain-level profiles were correlated with termite diet, as evidenced by higher relative abundances of Archaea in guts of soil-feeding termites, compared to those of wood-feeding species in the same family. The oligonucleotide probes also readily distinguished gut communities of wood-feeding taxa in the family Termitidae (higher termites) from those of other wood-feeding termite families (lower termites). The relative abundances of 16S-like archaeal rRNA in guts were positively correlated with rates of methane emission by live termites, and were consistent with previous work linking high. relative rates of methanogenesis with the soil (humus)-feeding habit. Probes for methanogenic Archaea detected members of only two families (Methanobacteriaceae and Methanosarcinaceae) in termite guts, and these typically accounted for 60% of the all archaeal probe signal. In four species of termites, Methanosarcinaceae were dominant, a novel observation for animal gut microbial communities, but no clear relationship was apparent between methanogen family profiles and termite diet or taxonomy. (C) 2001 Federation of European Microbiological Societies. Published by Elsevier Science B.V. All rights reserved. C1 IRD, F-78352 Jouy En Josas, France. INRA, UEPSD, F-78352 Jouy En Josas, France. Nat Hist Museum, Dept Entomol, London SW7 5BD, England. Queen Mary Univ London, Sch Biol Sci, London E1 4NS, England. Michigan State Univ, Dept Microbiol, E Lansing, MI 48824 USA. Michigan State Univ, Ctr Microbial Ecol, E Lansing, MI 48824 USA. Smithsonian Inst, Natl Museum Nat Hist, Lab Mol Systemat, Washington, DC 20560 USA. RP Kane, MD (reprint author), Natl Sci Fdn, Div Environm Biol, Room 635,4201 Wilson Blvd, Arlington, VA 22230 USA. EM mkane@nsf.gov RI brauman, alain/C-8400-2009 OI brauman, alain/0000-0002-4865-2919 NR 47 TC 72 Z9 77 U1 2 U2 19 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0168-6496 EI 1574-6941 J9 FEMS MICROBIOL ECOL JI FEMS Microbiol. Ecol. PD MAR PY 2001 VL 35 IS 1 BP 27 EP 36 DI 10.1016/S0168-6496(00)00108-2 PG 10 WC Microbiology SC Microbiology GA 411ZG UT WOS:000167529100004 ER PT J AU Campbell, BA AF Campbell, BA TI Radar backscatter from Mars: Properties of rock-strewn surfaces SO ICARUS LA English DT Article DE Mars; surface; radar ID LANDING SITE PREDICTIONS; DELAY-DOPPLER; SCATTERING AB Rock-strewn surfaces are apparently common on Mars, and radar backscatter data offer the most direct means for remotely estimating their statistical properties. This paper examines the height statistics of power-law and exponential rock size-frequency distributions, and demonstrates the dependence of root-mean-square (rms) height on horizontal scale as a function of the distribution parameters. In general, strewn surfaces have an inherent variation in roughness for horizontal length scales below the maximum rock diameter. This leads to variations in radar echo power with wavelength, even when the differential diameter function has an inverse-cubed power-law form. Size-frequency data for a rock-strewn test site in Hawaii are consistent, over a specific range of horizontal scales, with a power-law distribution. An exponential form, while better describing the rapid decline in rock abundance above a certain size threshold, underestimates the population at the smaller scales most relevant to radar scattering. Rock sphericity statistics, often cited in descriptions of rocky areas, appear to be consistent with a Rayleigh distribution of major and minor axis diameters about any chosen mean value. Depolarized backscatter data for the test site at 5.7-68 cm are proportional to the rms height at the wavelength scale, mirroring a similar trend for continuous rough rocky surfaces. An empirical model relating rms height to depolarized backscatter coefficient appears to well describe the behavior of strewn surfaces. The polarized echoes are consistent with Mie scattering from surface rocks for a reasonable choice of dielectric properties, but the number of free parameters and the interaction of the scatterer and surface yields weak remote-sensing roughness or dielectric constraints. While depolarized backscatter data provide robust estimates of the rms height for continuous and discrete roughness populations, their use in Mars landing site planning is model-dependent. For single-wavelength data, we cannot uniquely determine the size-frequency distribution and the maximum rock diameter. Dual-wavelength observations, in the S- to P-band range, may better constrain the surface properties. (C) 2001 Academic Press. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. NR 23 TC 13 Z9 14 U1 0 U2 1 PU ACADEMIC PRESS INC PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAR PY 2001 VL 150 IS 1 BP 38 EP 47 DI 10.1006/icar.2000.6566 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 421NY UT WOS:000168071500003 ER PT J AU Kawamura, J Tong, CYE Blundell, R Papa, DC Hunter, TR Patt, F Gol'tsman, G Gershenzon, E AF Kawamura, J Tong, CYE Blundell, R Papa, DC Hunter, TR Patt, F Gol'tsman, G Gershenzon, E TI Terahertz-frequency waveguide NbN hot-electron bolometer mixer SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT 2000 Applied Superconductivity Conference CY SEP 17-22, 2000 CL VIRGINIA BEACH, VIRGINIA DE superconducting receiver; hot-electron bolometer mixer; terahertz techniques ID RECEIVER; OPERATION; THZ AB We have developed a low-noise waveguide heterodyne receiver for operation near 1 THz using phonon-cooled NbN hot-electron boiometers, The mixer elements are submicron-sized microbridges of 4 nm-thick NbN film fabricated on a quartz substrate. Operating at a bath temperature of 4.2 K, the double-sideband receiver noise temperature is 760 K at 1.02 THz and 1100 K at 1.26 THz, The local oscillator is provided by solid-state sources, and power measured at the source is less than 1 muW The intermediate frequency bandwidth exceeds 2 GHz, The receiver was used to make the first ground-based heterodyne detection of a celestial spectroscopic line above 1 THz. C1 CALTECH, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Submillimeter Telescope Observ, Tucson, AZ 85721 USA. Moscow State Pedag Univ, Moscow 119435, Russia. RP Kawamura, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Tong, Edward/0000-0002-7736-4203; Hunter, Todd/0000-0001-6492-0090 NR 10 TC 16 Z9 17 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017-2394 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD MAR PY 2001 VL 11 IS 1 BP 952 EP 954 DI 10.1109/77.919505 PN 1 PG 3 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 425HP UT WOS:000168285400222 ER PT J AU Pisano, DA AF Pisano, DA TI Air power in the age of total war. SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Pisano, DA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGANIZATION AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47408 USA SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD MAR PY 2001 VL 87 IS 4 BP 1563 EP 1564 DI 10.2307/2674870 PG 2 WC History SC History GA 416RK UT WOS:000167793800148 ER PT J AU Smith, BD AF Smith, BD TI Low-level food production SO JOURNAL OF ARCHAEOLOGICAL RESEARCH LA English DT Article DE food production; domestication; origins of agriculture; subsistence economy ID EASTERN NORTH-AMERICA; INITIAL DOMESTICATION AB Societies with low-level food production economies occupy the vast and diverse middle ground between hunting-fishing-foraging and agriculture. Efforts by Ford, Harris, Rindos, Zvelebil, and others to characterize this 'in-between' territory are discussed, and a new conceptual framework is proposed. Domestication, the central landmark of this middle ground, is situated well away from the boundaries with hunting-gathering and agriculture, and separates low-level food production economies into two broad categories. Key issues and questions concerning societies with low-level food production, both with and without domesticates, are discussed. Hunter-gatherer and agriculture boundary zones on either side of the middle ground are considered, as one the developmental pathways that traverse them. C1 Smithsonian Inst, Museum Hist Nat, Washington, DC 20560 USA. RP Smith, BD (reprint author), Smithsonian Inst, Museum Hist Nat, Washington, DC 20560 USA. EM smith.bruce@nmnh.si.edu NR 91 TC 206 Z9 211 U1 1 U2 14 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1059-0161 J9 J ARCHAEOL RES JI J. Archaeol. Res. PD MAR PY 2001 VL 9 IS 1 BP 1 EP 43 DI 10.1023/A:1009436110049 PG 43 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 434VY UT WOS:000168837600001 ER PT J AU Reinhardt, EG Stanley, DJ Schwarcz, HP AF Reinhardt, EG Stanley, DJ Schwarcz, HP TI Human-induced desalinization of Manzala lagoon, Nile delta, Egypt: Evidence from isotopic analysis of benthic invertebrates SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE Aswan High Dam; fisheries; invertebrate fauna; strontium; oxygen and carbon isotopes; Manzala lagoon; molluscs; Nile delta; salinity; Nile River ID SAN-FRANCISCO BAY; BRACKISH WATERS; STABLE-ISOTOPE; STRONTIUM; PALEOSALINITY; MARINE; SR-87/SR-86; CALIFORNIA; ESTUARINE; RECORD AB This study combines isotopic (Sr-87/Sr-86, delta O-18 and delta C-13) With paleontological data to derive a paleosalinity proxy in order to determine the impact of the Aswan High Dam on Manzala lagoon in Egypt's Nile delta. Analyses were made on 17 invertebrate taxa (molluscs, crustaceans, foraminifera, serpulid worms). These were collected in 17 surficial samples and 18 samples from two cores collected at the two salinity extremes of the lagoon. Of the three isotopic systems, Sr isotopes (Sr-87/Sr-86) best record salinity changes within the lagoon. The main control on C isotopes within shell material is the mixing of fresh and marine waters entering the lagoon; thus it is also a useful paleosalinity indicator. The oxygen isotopic composition of shells increased with decreasing salinity: this is consistent with the observation that fresh waters feeding the lagoon are enriched in O-18 with respect to Mediterranean seawater. However, the gradient in delta O-18 between these end-members is not sufficient to allow us to use O isotopes as a recorder of paleosalinity. Sr isotopes fi om a core on the landward margin of the lagoon documents a decreased salinity shift from approximately 4-13 ppt to 1-2 ppt since about 1950. The major reduction of salinity in Manzala is due to a dramatic increase in freshwater discharge from drains into the lagoon and effects of Aswan High Dam closure in 1964. This salinity change has been the most significant in the past 100 years. This method, combining paleontological and isotopic analyses of sediment cores, provides documentation of environmental deterioration and thus holds promise for the study of anthropogenically-induced salinity changes in other deltaic systems from around the world. C1 McMaster Univ, Sch Geol & Geophys, Hamilton, ON L8S 4M1, Canada. Smithsonian Inst, Deltas Global Change Program, Washington, DC 20560 USA. RP Reinhardt, EG (reprint author), McMaster Univ, Sch Geol & Geophys, Hamilton, ON L8S 4M1, Canada. NR 54 TC 15 Z9 16 U1 2 U2 9 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD SPR PY 2001 VL 17 IS 2 BP 431 EP 442 PG 12 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 443AJ UT WOS:000169316900018 ER PT J AU Johnson, DW Hungate, BA Dijkstra, P Hymus, G Drake, B AF Johnson, DW Hungate, BA Dijkstra, P Hymus, G Drake, B TI Effects of elevated carbon dioxide on soils in a Florida scrub oak ecosystem SO JOURNAL OF ENVIRONMENTAL QUALITY LA English DT Article ID ION-EXCHANGE RESIN; PONDEROSA PINE; ATMOSPHERIC CO2; NITROGEN-FERTILIZATION; N FERTILIZATION; LITTER; DECOMPOSITION; RESPIRATION; ENRICHMENT; RESPONSES AB The results of a 3-yr study on the effects of elevated CO2 on soil N and P, soil pCO(2), and calculated CO2 efflux in a fire-regenerated Florida scrub oak ecosystem are summarized. We hypothesized that elevated CO2 would cause (i) increases in soil pCO(2) and soil respiration and (ii) reduced levels of soil-available N and P. The effects of elevated CO2 on soil N availability differed according to the method used. Results of resin lysimeter collections and anion exchange membrane tests in the field showed reduced NO3- in soils in Years 1 and 3. On the other hand, re-analysis of homogenized, buried soil bags after 1 yr suggested a relative increase in N availability (lower C to N ratio) under elevated CO2. In the case of P, the buried bags and membranes suggested a negative effect of CO2 on P during the first year; this faded over time, however, as P availability declined overall, probably in response to P uptake. Elevated CO2 had no effect on soil pCO(2) or calculated soil respiration at any time, further suggesting that plant rather than microbial uptake was the primary factor responsible for the observed changes in N and P availability with elevated CO2. C1 Univ Nevada, Coll Agr, Reno, NV 89512 USA. No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. Plant Protect Serv, NL-6700 HC Wageningen, Netherlands. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Johnson, DW (reprint author), Univ Nevada, Coll Agr, Reno, NV 89512 USA. RI Hungate, Bruce/F-8991-2011 OI Hungate, Bruce/0000-0002-7337-1887 NR 42 TC 39 Z9 39 U1 0 U2 8 PU AMER SOC AGRONOMY PI MADISON PA 677 S SEGOE RD, MADISON, WI 53711 USA SN 0047-2425 J9 J ENVIRON QUAL JI J. Environ. Qual. PD MAR-APR PY 2001 VL 30 IS 2 BP 501 EP 507 PG 7 WC Environmental Sciences SC Environmental Sciences & Ecology GA 445JY UT WOS:000169455400025 PM 11285911 ER PT J AU Mulhern, DM Ubelaker, DH AF Mulhern, DM Ubelaker, DH TI Differences in osteon banding between human and nonhuman bone SO JOURNAL OF FORENSIC SCIENCES LA English DT Article; Proceedings Paper CT 52nd Annual Meeting of the American-Academy-of-Forensic-Sciences CY FEB, 2000 CL RENO, NEVADA SP Amer Acad Forens Sci DE forensic science; forensic anthropology; histology; bone; Haversian system AB The objective of this paper is to compare patterns of osteon organization in human and nonhuman bone. A linear organization of Haversian systems in nonhuman bone, where osteons line up in rows, has been reported but has not been quantified. The present research provides a quantitative examination of this observation through a comparative analysis of the femoral midshaft from human and nonhuman bone. Femoral midshaft thin sections from 60 humans were compared to femoral midshaft sections from nine sheep and six miniature swine. The presence or absence of osteon banding was recorded and, if present, described. Results indicate that 2 out of 60 human sections and 5 out of 15 nonhuman sections exhibit osteon banding (chi (2) = 9.46; P < 0.01). Further. the type of banding present in the human and nonhuman samples is easily distinguished, indicating that human and nonhuman bone can be distinguished where banding is present in this study. C1 Natl Museum Nat Hist, Smithsonian Inst, MRC 112, Dept Anthropol, Washington, DC 20560 USA. RP Mulhern, DM (reprint author), Natl Museum Nat Hist, Smithsonian Inst, MRC 112, Dept Anthropol, 10th St & Constitut Ave NW, Washington, DC 20560 USA. NR 7 TC 37 Z9 39 U1 2 U2 9 PU AMER SOC TESTING MATERIALS PI W CONSHOHOCKEN PA 100 BARR HARBOR DR, W CONSHOHOCKEN, PA 19428-2959 USA SN 0022-1198 J9 J FORENSIC SCI JI J. Forensic Sci. PD MAR PY 2001 VL 46 IS 2 BP 220 EP 222 PG 3 WC Medicine, Legal SC Legal Medicine GA 451JB UT WOS:000169798000003 PM 11305421 ER PT J AU Yoder, C Ubelaker, DH Powell, JF AF Yoder, C Ubelaker, DH Powell, JF TI Examination of variation in sternal rib end morphology relevant to age assessment SO JOURNAL OF FORENSIC SCIENCES LA English DT Article; Proceedings Paper CT 51st Annual Meeting of the American-Academy-of-Forensic-Sciences CY FEB 15-21, 1999 CL ORLANDO, FLORIDA SP Amer Acad Forens Sci DE forensic science; forensic anthropology; physical anthropology; age assessment; sternal rib ID PHASE-ANALYSIS; INTERCOSTAL VARIATION AB The morphology of the sternal end of the right fourth rib has been proffered as an accurate age assessor in skeletonized individuals of both sexes. This technique was tested for its applicability on left and right II, III, V-IX. Tests were performed between phase scores obtained from right and left ribs; right rib IV phase scores and scores obtained from the others in the right rib series; and between right rib IV scores and a composite score composed of the average of an individual's phase scores (omitting rib IV). Left ribs IV-IX were found not to vary significantly from their right counterparts. Although only right rib II was found to vary significantly from rib IV, use of the other ribs in the series should be undertaken with caution due to questions concerning their statistical significance. A composite score is therefore recommended for use instead. C1 Texas A&M Univ, Dept Anthropol, College Stn, TX 77843 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. Univ New Mexico, Dept Anthropol, Albuquerque, NM 87131 USA. RP Yoder, C (reprint author), Texas A&M Univ, Dept Anthropol, College Stn, TX 77843 USA. NR 25 TC 18 Z9 19 U1 0 U2 5 PU AMER SOC TESTING MATERIALS PI W CONSHOHOCKEN PA 100 BARR HARBOR DR, W CONSHOHOCKEN, PA 19428-2959 USA SN 0022-1198 J9 J FORENSIC SCI JI J. Forensic Sci. PD MAR PY 2001 VL 46 IS 2 BP 223 EP 227 PG 5 WC Medicine, Legal SC Legal Medicine GA 451JB UT WOS:000169798000004 PM 11305422 ER PT J AU Schneider, CJ Losos, JB de Queiroz, K AF Schneider, CJ Losos, JB de Queiroz, K TI Evolutionary relationships of the Anolis bimaculatus group from the northern Lesser Antilles SO JOURNAL OF HERPETOLOGY LA English DT Article ID CYTOCHROME-B GENE; CHARACTER-DISPLACEMENT; TERRITORY ACQUISITION; MICROGEOGRAPHIC VARIATION; LIZARD POPULATIONS; MITOCHONDRIAL-DNA; WEST-INDIES; OCULATUS; TREES; SIZE AB Lizards in the Anolis bimaculatus group from the northern Lesser Antilles have played an important role in theoretical and empirical developments in ecology, behavior, and evolution over the last four decades. Despite intense interest, the lack of a formal phylogenetic analysis for the bimaculatus group has limited comparative and historical evolutionary analyses. Here we present a phylogenetic analysis of species relationships within the bimaculatus group based on separate and combined analyses of mitochondrial DNA and previously published allozyme data. These analyses indicate that (1) the wattsi group of small anoles is a basal, well-supported monophyletic group; (2) the large anoles A. bimaculatus and A. leachi are not sister species-rather, there is a well-supported sister relationship between A. bimaculatus and A. gingivinus; (3) the A. marmoratus complex from the Guadeloupean archipelago is deeply differentiated and paraphyletic, with A. sabanus, A. lividus, and possibly A. oculatus nested within it; (4) the phylogenetic position of A. leachi is not well resolved, but a combined analysis of mtDNA and allozyme data favor placing A. leachi as the sister taxon to the (A. marmoratus, A. lividus, A. sabanus, A. oculatus) group; and (5) the phylogenetic position of A. nubilus remains uncertain pending additional data. The proposed phylogeny elucidates the evolutionary history and biogeography of the bimaculatus group and allows a reassessment of the character displacement and taxon cycle/loop hypotheses. C1 Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. Boston Univ, Dept Biol, Boston, MA 02215 USA. Washington Univ, Dept Biol, St Louis, MO 63130 USA. Smithsonian Inst, Museum Natl Hist Nat, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Schneider, CJ (reprint author), Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. NR 72 TC 29 Z9 35 U1 1 U2 4 PU SOC STUDY AMPHIBIANS REPTILES PI ST LOUIS PA C/O ROBERT D ALDRIDGE, ST LOUIS UNIV, DEPT BIOLOGY, 3507 LACLEDE, ST LOUIS, MO 63103 USA SN 0022-1511 J9 J HERPETOL JI J. Herpetol. PD MAR PY 2001 VL 35 IS 1 BP 1 EP 12 DI 10.2307/1566016 PG 12 WC Zoology SC Zoology GA 413BE UT WOS:000167589400001 ER PT J AU Ovaska, K Rand, AS AF Ovaska, K Rand, AS TI Courtship and reproductive behavior of the frog Eleutherodactylus diastema (Anura : Leptodactylidae) in Gamboa, Panama SO JOURNAL OF HERPETOLOGY LA English DT Article ID BRITISH-VIRGIN-ISLANDS; MATING-BEHAVIOR; JOHNSTONEI AB Courtship behavior has been documented in detail for only a few species of Eleutherodactylus, all from the Puerto Rico bank. Here we report on courtship, calling, nest sites, and egg clutches of Eleutherodactylus diastema from Gamboa, Panama. In fury 1999, we observed five natural and four staged courtships in the natural habitat. The courtship consisted of an approach by a female, a visual-tactile display when the pair first made contact, and a phase when the male led the female to an oviposition site. Within the first 2 min after contact the male bumped the female 9-12 times with his partly inflated vocal sac, most bumps being initiated by an approach by the female. The male then led the female to a nest site located within his calling territory. Oviposition took place in a variety of concealed or partially concealed sites between leaves or plant stems or inside a bromeliad. Once we observed an agonistic interaction between two females competing for a male in his nest site. Four of the five nests located contained multiple clutches in different developmental stages tone nest had seven clutches and three each had three clutches). We detected no parental care. This study revealed three particularly interesting aspects of the reproductive behavior of E. diastema: the occurrence of a visual-tactile bumping display at the beginning of the courtship female-female competition for mates, and repeated use of nest sites by individual males. C1 Biolinx Environm Res Ltd, Victoria, BC V8Z 6M1, Canada. Univ British Columbia, Dept Forest Sci, Vancouver, BC V6T 1Z4, Canada. Smithsonian Trop Res Inst, Balboa, Panama. RP Ovaska, K (reprint author), Biolinx Environm Res Ltd, 4180 Clinton Pl, Victoria, BC V8Z 6M1, Canada. NR 20 TC 14 Z9 15 U1 0 U2 1 PU SOC STUDY AMPHIBIANS REPTILES PI ST LOUIS PA C/O ROBERT D ALDRIDGE, ST LOUIS UNIV, DEPT BIOLOGY, 3507 LACLEDE, ST LOUIS, MO 63103 USA SN 0022-1511 J9 J HERPETOL JI J. Herpetol. PD MAR PY 2001 VL 35 IS 1 BP 44 EP 50 DI 10.2307/1566021 PG 7 WC Zoology SC Zoology GA 413BE UT WOS:000167589400006 ER PT J AU Blackwell, BAB Fevrier, S Blickstein, JIB Paddayya, K Perraglia, M Jhaldiyal, R Skinner, AR AF Blackwell, BAB Fevrier, S Blickstein, JIB Paddayya, K Perraglia, M Jhaldiyal, R Skinner, AR TI ESR dating of an Acheulean quarry site at Isampur, India SO JOURNAL OF HUMAN EVOLUTION LA English DT Meeting Abstract C1 Williams Coll, Dept Chem, Williamstown, MA 01267 USA. RFK Summer Res Inst, Flushing, NY 11366 USA. Deccan Coll, Dept Archaeol, Pune 411006, Maharashtra, India. Smithsonian Inst, Museum Natl Hist Nat, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 10 Z9 10 U1 0 U2 1 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD MAR PY 2001 VL 40 IS 3 BP A3 EP A3 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 407CR UT WOS:000167254300008 ER PT J AU Ditchfield, P Ferraro, J Plummer, T Bishop, L Potts, R AF Ditchfield, P Ferraro, J Plummer, T Bishop, L Potts, R TI An early secondary grassland with hominid activities at Kanjera South, Kenya SO JOURNAL OF HUMAN EVOLUTION LA English DT Meeting Abstract C1 Univ Bristol, Dept Geol, Bristol BS8 1RJ, Avon, England. Univ Calif Los Angeles, Dept Anthropol, Los Angeles, CA 90095 USA. CUNY Queens Coll, Dept Anthropol, Flushing, NY 11367 USA. Liverpool John Moores Univ, Liverpool L3 3AF, Merseyside, England. Smithsonian Inst, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD MAR PY 2001 VL 40 IS 3 BP A7 EP A7 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 407CR UT WOS:000167254300014 ER PT J AU Silverman, NJ Schwartz, GT Wood, B AF Silverman, NJ Schwartz, GT Wood, B TI Are the P(4)s of Paranthropus uniquely molarized? SO JOURNAL OF HUMAN EVOLUTION LA English DT Meeting Abstract C1 George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD MAR PY 2001 VL 40 IS 3 BP A21 EP A21 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 407CR UT WOS:000167254300035 ER PT J AU Boardman, RS AF Boardman, RS TI The growth and function of skeletal diaphragms in the colony life of tower Paleozoic Trepostomata (Bryozoa) SO JOURNAL OF PALEONTOLOGY LA English DT Article AB In many species of lower Paleozoic trepostomes (Bryozoa; class Stenolaemata) transverse partitions called skeletal diaphragms differentiated feeding from non-feeding regions of colonies. It has been thought that each diaphragm floored the living chamber of a feeding polypide. However, analysis of skeletal growth patterns has shown that many diaphragms were too close to colony surfaces or too closely spaced in ontogenetic sequences to have accommodated feeding polypides at any given life horizon. Apparently colonies were capable of maintenance and even robust growth with reduced numbers of active polypides, an interpretation supported by comparison with living stenolaemates. A synthesis of the inferred functions of colonies of the extinct trepostomes with post-Triassic fossil and living stenolaemates suggests that walls of trepostome autozooids grew continuously outward so that living chambers starting from their basal diaphragms ranged from shallow to full sized on colony surfaces. Under-sized polypides apparently grew with their under-sized living chambers and fed as they regenerated to full size, as in living stenolaemates. Actively feeding colony surfaces included autozooids either having polypides at similar or different stages of polypide regeneration, or fully regenerated. Nonfeeding colony surfaces included autozooids either having degenerated polypides, autozooids with diaphragms too closely spaced to skeletal apertures to have housed polypides, or possibly, autozooids that stopped skeletal growth in proximal regions of some large colonies. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Boardman, RS (reprint author), 3612 E Forest Lake Dr, Sarosta, FL 34232 USA. NR 30 TC 6 Z9 6 U1 0 U2 0 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD MAR PY 2001 VL 75 IS 2 BP 225 EP 240 DI 10.1666/0022-3360(2001)075<0225:TGAFOS>2.0.CO;2 PG 16 WC Paleontology SC Paleontology GA 415JL UT WOS:000167718000001 ER PT J AU DiMichele, WA Mamay, SH Chaney, DS Hook, RW Nelson, WJ AF DiMichele, WA Mamay, SH Chaney, DS Hook, RW Nelson, WJ TI An early Permian flora with Late Permian and Mesozoic affinities from north-central Texas SO JOURNAL OF PALEONTOLOGY LA English DT Article ID MASS EXTINCTION; PALEOBOTANY; TRANSITION; PALYNOLOGY; MORPHOLOGY; CONIFER; CRISIS; LAND AB Early Permian (late Leonardian Series) plant assemblages from King, Knox, and Stonewall Counties of North-Central Texas are dominated by seed plants, some apparently congeneric with taxa heretofore known only from the Late Permian or the Mesozoic. Conifers are the dominant elements, including one or more species of Ullmannia, Pseudovoltzia liebeana, both known from thr Late Permian Zechstein flora of Germany and England, Podozamites sp., characteristic of the Mesozoic. and Walchia sp., abundant in Early Permian floras. Locally common are Taeniopteris cf. eckardtii, a Zechstein species, an unidentified plant represented by pinnule-like laminae with fine parallel veins, similar to pinnules of some Mesozoic cycads, and calamite stems. Rarely encountered are leaf fragments of the Paleozoic ginkgophyte Dicranophyllum, flabellate ginkgophyte leaves, leaves with a broad midvein and narrow, fimbriate lamina, and Wattia, typical of the Early Permian. Associated with these foliar remains are ovulate reproductive structures including the presumed cycad megasporophyll Dioonitocarpidim, known only from the Mesozoic, a voltzialean cone scale similar to Swedenborgia, and a variety of seeds, some remarkably similar to Agathis, of Cretaceous age. The assemblage includes only rare scraps of foliage and seeds possibly attributable to the pteridophyllous elements (gigantopterids, callipterids, and ferns) that dominate the Permian. The fossil plants occur in multistorey, fining-upwards, tidal-channel deposits that also include pelecypods and fragmentary palaeoniscoid fish. The occurrence of derived lineages in xeric habitats during the Early Permian indicates that some supposed Mesozoic groups actually preceded and survived the end-Permian extinction, reappearing in basinal lowlands during the mid-Mesozoic. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. Univ Texas, Texas Mem Museum, Austin, TX 78758 USA. Illinois State Geol Survey, Champaign, IL 61820 USA. RP DiMichele, WA (reprint author), Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RI DiMichele, William/K-4301-2012 NR 56 TC 54 Z9 57 U1 2 U2 9 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD MAR PY 2001 VL 75 IS 2 BP 449 EP 460 DI 10.1666/0022-3360(2001)075<0449:AEPFWL>2.0.CO;2 PG 12 WC Paleontology SC Paleontology GA 415JL UT WOS:000167718000019 ER PT J AU Li, AS Stoecker, DK Coats, DW AF Li, AS Stoecker, DK Coats, DW TI Use of the 'food vacuole content' method to estimate grazing by the mixotrophic dinoflagellate Gyrodinium galatheanum on cryptophytes SO JOURNAL OF PLANKTON RESEARCH LA English DT Article ID CLEARANCE RATE-CONSTANT; CHESAPEAKE-BAY; PARAMECIUM-TETRAURELIA; GYMNODINIUM-SANGUINEUM; PLANKTONIC COPEPODS; TEMPORAL ASPECTS; LIGHT-INTENSITY; FEEDING RATES; RED-TIDE; GROWTH AB We measured in situ grazing rates of the mixotrophic dinoflagellate Gyrodinium galatheanum (Braarud) Taylor 1995 on populations of phycoerythrin-containing cryptophytes in Chesapeake Bay. Rates were estimated from instantaneous food vacuole contents, in situ temperatures, cryptophyte abundances and experimentally determined digestion rates. Laboratory digestion experiments showed that specific digestion rate constants increased sigmoidally with temperature, but were unrelated to the initial food vacuole content when it was <0.46 cryptophytes dinoflagellate (1). These results allowed us to establish an empirical model to estimate in situ ingestion of cryptophyte prey by G. galatheanum. The estimated rates ranged from 0 to 0.26 cryptophytes dinoflagellate (1) day (1), corresponding to daily ingestion of 0-12.29 pg carbon, 0-2.48 pg nitrogen and 0-0.34 pg phosphorus dinoflagellate (1). Estimated daily consumption of cryptophyte biomass by G. galatheanum was equivalent to 0-12% of body carbon, 0-13% of body nitrogen and 0-21% of body phosphorus. Estimated in situ clearance rates for cryptophytes ranged from 0 to 0.27 l dinoflagellate (1) day (1), representing daily removal of 0-4% of the cryptophyte standing stock. Although G. galatheanum may increase its growth rate through phagotrophy, it appears to have little grazing impact on cryptophyte prey populations. C1 Univ Maryland, Horn Point Environm Lab, Ctr Environm Sci, Cambridge, MD 21613 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Li, AS (reprint author), Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA. RI stoecker, diane/F-9341-2013 NR 54 TC 13 Z9 14 U1 1 U2 9 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0142-7873 EI 1464-3774 J9 J PLANKTON RES JI J. Plankton Res. PD MAR PY 2001 VL 23 IS 3 BP 303 EP 318 DI 10.1093/plankt/23.3.303 PG 16 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 430LE UT WOS:000168574700007 ER PT J AU Polhemus, DA Polhemus, JT AF Polhemus, DA Polhemus, JT TI A revision of the genus Ptilomera (Heteroptera : Gerridae) on New Guinea and nearby islands SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY LA English DT Article AB The genus Ptilomera is revised for New Guinea and nearby islands. Four previously described taxa are redescribed and discussed: P. aello Breddin, P. papuensis Hungerford & Matsuda, P. breddini Hungerford & Matsuda, and P, cheesmanae Hungerford & Matsuda, the latter newly elevated from subspecies to full species rank. Eighteen new species are described as follows: P. waigeo from Waigeo Island, P. misoolensis from Misool Island, P. yapenana from Yapen Island, P. arfak from the Vogelkop Peninsula of Irian Jaya, P. timika from southern Irian Jaya, P, etna from western central Irian Jaya, P. iriana from north central Irian Jaya, P. wapoga from north central Irian Jaya, P. kiunga from southwestern Papua New Guinea. P. omo from southern central Papua New Guinea, P. kutubu from the southern highlands of Papua New Guinea. P. jimi from the central highlands of Papua New Guinea, P. wewak from northern Papua New Guinea. P. morobe from northeastern Papua New Guinea, P. biroi from northeastern Papua New Guinea, P. insularis from Umboi Island, P. novabrittanica from New Britain. and P. bismarckensis from New Ireland. Keys to all species occurring in the New Guinea region are provided fur both males and females, accompanied by range maps, and figures of the male genitalic complex, male parameres, male endosuma, and female terminal abdomen in lateral view. C1 Smithsonian Inst, Dept Entomol, MRC 105, Washington, DC 20560 USA. RP Polhemus, DA (reprint author), Smithsonian Inst, Dept Entomol, MRC 105, NHB 169, Washington, DC 20560 USA. NR 39 TC 4 Z9 5 U1 1 U2 2 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 0028-7199 J9 J NEW YORK ENTOMOL S JI J. N.Y. Entomol. Soc. PD SPR PY 2001 VL 109 IS 1 BP 81 EP 166 DI 10.1664/0028-7199(2001)109[0081:AROTGP]2.0.CO;2 PG 86 WC Entomology SC Entomology GA 451WZ UT WOS:000169826700003 ER PT J AU Citino, SB Bush, M Grobler, D Lance, W AF Citino, SB Bush, M Grobler, D Lance, W TI Anaesthesia of roan antelope (Hippotragus equinus) with a combination of A3080, medetomidine and ketamine SO JOURNAL OF THE SOUTH AFRICAN VETERINARY ASSOCIATION-TYDSKRIF VAN DIE SUID-AFRIKAANSE VETERINERE VERENIGING LA English DT Article DE A3080; anaesthesia; atipamezole; Hippotragus equinus; ketamine; medetomidine; naltrexone; roan antelope ID ORYX ORYX-LEUCORYX; IMMOBILIZATION AB A dose range was determined for anaesthesia of 20 recently boma-captured roan antelope (Hippotragus equinus) with the synthetic opiate A3080 combined with medetomidine and ketamine. A dose of 10-30 mu /kg A3080 ((x) over bar = 20 +/- 8 mug/kg) combined with 5-21 mug/kg medetomidine ((x) over bar = 13 +/- 7 mug/kg) plus 0.29-1.11 mg/kg ketamine ((x) over bar = 0.71 +/- 0.24 mg/kg) was found to be safe and effective for the field conditions in this study. The anaesthesia produced by this drug combination was predictable and characterised by a short induction time, good muscle relaxation, and acceptable physiological parameters for anaesthesia periods ranging from 49-103 min ((x) over bar = 64 +/- 19 min). The wide range (3-4-fold) of doses with acceptable results is also an indication that this drug combination has a wide margin of safety in roan antelope, making it desirable for field use. When 2 dose levels (2-3-fold difference) were retrospectively evaluated, no statistical difference was found in induction times, and no observable clinical differences in the anaesthetic episodes were seen. Based on this study, the recommended dose range in roan antelope for this combination is 10-13 mug/kg A3080, 5-6 mug/kg medetomidine and 0.3-0.6 mg/kg ketamine. The anaesthesia produced by this combination was rapidly and completely reversed by i.m. or i.v. injections of naltrexone at 30 times the A3080 dose ((x) over bar = 0.60 +/- 0.25 mg/kg) and atipamezole at 3 times the medetomidine dose ((x) over bar = 38 +/- 20 mug/kg). No residual effects from ketamine were noted following reversal of A3080 and medetomidine. No mortality was associated with this protocol. C1 White Oak Conservat Ctr, Yulee, FL 32097 USA. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. S African Natl Pk, ZA-1350 Skukuza, South Africa. Wildlife Pharmaceut Inc, Ft Collins, CO 80524 USA. RP Citino, SB (reprint author), White Oak Conservat Ctr, 3823 Owens Rd, Yulee, FL 32097 USA. NR 19 TC 18 Z9 20 U1 0 U2 1 PU SOUTH AFRICAN VET ASSN PI MONUMENT PARK PA PO BOX 25033, MONUMENT PARK 0105, SOUTH AFRICA SN 0038-2809 J9 J S AFR VET ASSOC JI J. S. Afr. Vet. Assoc.-Tydskr. Suid-Afr. Vet. Ver. PD MAR PY 2001 VL 72 IS 1 BP 29 EP 32 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA 424PA UT WOS:000168239600007 PM 11563714 ER PT J AU Engelbrecht, BMJ Herz, HM AF Engelbrecht, BMJ Herz, HM TI Evaluation of different methods to estimate understorey light conditions in tropical forests SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE fisheye photography; hemispherical photography; light measurement; plant canopy analysis; PPFD; spherical densiometer ID SOLAR-RADIATION; RAIN-FOREST; ENVIRONMENTS; PHOTOGRAPHS; REGIMES AB The suitability of several methods for estimating light conditions in the understorey of tropical forests, and of different sampling schedules was evaluated. Eight conditions at 16 understorey sites in a Panamanian loll land forest were continuously measured for 9 mo with quantum sensors and photodiodes. Light conditions at the sites were also assessed indirectly with hemispherical fisheye photographs, plant canopy analysis, SX-mm photographs, 24-mm photographs and a spherical densiometer. Estimates from all indirect methods, except the spherical densiometer, were highly correlated with the direct measurements. Short-term direct light measurements for a day or a week also correlated with long-term light conditions. The indirect measures differed by up to c. 70% from the direct measures relative to single site measurements. Hence, the indirect methods are inadequate where single site light conditions have to be assessed accurately. However, because light conditions encountered in the understorey varied up to 13-fold, the indirect methods were found to be well suited to rank understorey light conditions among a large number of sites. The results from frequent and infrequent sampling schedules differed only slightly, suggesting that taking indirect measures at the beginning and the end of a study offers a reasonable compromise between accuracy and sampling effort. C1 Tech Univ Darmstadt, Inst Bot, Fachbereich Biol, D-64287 Darmstadt, Germany. Univ Bielefeld, Lehrstuhl Expt Okol & Okosystembiol, D-33615 Bielefeld, Germany. RP Engelbrecht, BMJ (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. RI Engelbrecht, Bettina/E-9914-2012 NR 22 TC 65 Z9 66 U1 2 U2 16 PU CAMBRIDGE UNIV PRESS PI PORT CHESTER PA 110 MIDLAND AVE, PORT CHESTER, NY 10573-4930 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD MAR PY 2001 VL 17 BP 207 EP 224 PN 2 PG 18 WC Ecology SC Environmental Sciences & Ecology GA 418XW UT WOS:000167920700004 ER PT J AU Jacobson, ER Origgi, F Pessier, AP Lamirande, EW Walker, I Whitaker, B Stalis, IH Nordhausen, R Owens, JW Nichols, DK Heard, D Homer, B AF Jacobson, ER Origgi, F Pessier, AP Lamirande, EW Walker, I Whitaker, B Stalis, IH Nordhausen, R Owens, JW Nichols, DK Heard, D Homer, B TI Paramyxovirus infection in caiman lizards (Draecena guianensis) SO JOURNAL OF VETERINARY DIAGNOSTIC INVESTIGATION LA English DT Article ID OPHIDIAN PARAMYXOVIRUS; SNAKES; VIRUS; COLLECTION; PNEUMONIA AB Three separate epidemics occurred in caiman lizards (Dracaena guianensis) that were imported into the USA from Peru in late 1998 and early 1999. Histologic evaluation of tissues from necropsied lizards demonstrated a proliferative pneumonia. Electron microscopic examination of lung tissue revealed a virus that was consistent with members of the family Paramyxoviridae. Using a rabbit polyclonal antibody against an isolate of ophidian (snake) paramyxovirus, an immunoperoxidase staining technique demonstrated immunoreactivity within pulmonary epithelial cells of I lizard. Homogenates. of lung, brain, liver, or kidney from affected lizards were placed in flasks containing monolayers of either terrapene heart cells or viper heart cells. Five to 10 days later, syncytial cells formed. When Vero cells were inoculated with supernatant of infected terrapene heart cells, similar syncytial. cells developed. Electron microscopic evaluation of infected terrapene heart cells revealed intracytoplasmic inclusions consisting of nucleocapsid strands. Using negative-staining electron microscopy, abundant filamentous nucleocapsid material with a herringbone structure typical of the Paramyxoviridae was observed in culture medium of infected viper heart cells. Seven months following the initial epizootic, blood samples were collected from surviving group 1 lizards, and a hemagglutination inhibition assay was performed to determine presence of specific antibody against the caiman lizard isolate. Of the 17 lizards sampled, 7 had titers of less than or equal to1:20 and 10 had titers of >1:20 and less than or equal to1:80. This report is only the second of a paramyxovirus identified in a lizard and is the first to snow the relationship between histologic and ultrastructural findings and virus isolation. C1 Univ Florida, Coll Vet Med, Gainesville, FL 32610 USA. Zool Soc San Diego, Dept Pathol, San Diego, CA 92112 USA. Smithsonian Inst, Natl Zool Pk, Dept Pathol, Washington, DC 20008 USA. Natl Aquarium, Baltimore, MD 21202 USA. Calif Vet Diagnost Lab Syst, Davis, CA 95616 USA. NIH, Vet Resources Program, Off Res Serv, Bethesda, MD 20892 USA. RP Jacobson, ER (reprint author), Univ Florida, Coll Vet Med, Gainesville, FL 32610 USA. NR 18 TC 19 Z9 20 U1 0 U2 4 PU AMER ASSOC VETERINARY LABORATORY DIAGNOSTICIANS INC PI TURLOCK PA PO BOX 1522, TURLOCK, CA 95381 USA SN 1040-6387 J9 J VET DIAGN INVEST JI J. Vet. Diagn. Invest. PD MAR PY 2001 VL 13 IS 2 BP 143 EP 151 PG 9 WC Veterinary Sciences SC Veterinary Sciences GA 458XQ UT WOS:000170221100008 PM 11289210 ER PT J AU Mikota, SK Peddie, L Peddie, J Isaza, R Dunker, F West, G Lindsay, W Larsen, RS Salman, MD Chatterjee, D Payeur, J Whipple, D Thoen, C Davis, DS Sedgwick, C Montali, RJ Ziccardi, M Maslow, J AF Mikota, SK Peddie, L Peddie, J Isaza, R Dunker, F West, G Lindsay, W Larsen, RS Salman, MD Chatterjee, D Payeur, J Whipple, D Thoen, C Davis, DS Sedgwick, C Montali, RJ Ziccardi, M Maslow, J TI Epidemiology and diagnosis of Mycobacterium tuberculosis in captive Asian elephants (Elephas maximus) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE elephant; Elephas maximus; Loxodonta africana; tuberculosis; Mycobacterium tuberculosis; tuberculin test ID RESPIRATORY SPECIMENS; AMPLIFICATION; POLYMORPHISM; INFECTION; ANIMALS; COMPLEX; BOVIS; PCR AB The deaths of two Asian elephants (Elephas maximus) in August 1996 led the United States Department of Agriculture to require the testing and treatment of elephants for tuberculosis. From August 1996 to September 1999, Mycobacterium tuberculosis infection was confirmed by culture in 12 of 118 elephants in six herds. Eight diagnoses were made antemortem on the basis of isolation of M. tuberculosis by culture of trunk wash samples', the remainder (including the initial two) were diagnosed postmortem. We present the case histories, epidemiologic characteristics, diagnostic test results, and therapeutic plans from these six herds. The intradermal tuberculin test, enzyme-linked immunosorbent assay serology, the blood tuberculosis test, and nucleic acid amplification and culture are compared as methods to diagnose M. tuberculosis infection in elephants. C1 Univ Penn, Philadelphia, PA 19104 USA. Vet Affairs Med Ctr, Infect Dis Sect, Philadelphia, PA 19104 USA. Lincoln Pk Zoo, Chicago, IL 60614 USA. Smithsonian Natl Zool Pk, Washington, DC 20008 USA. Los Angeles Zoo, Los Angeles, CA 90027 USA. Texas A&M Univ, Dept Vet Pathobiol, College Stn, TX 77843 USA. Iowa State Univ Sci & Technol, Coll Vet Med, Dept Microbiol Immunol & Prevent Med, Ames, IA 50011 USA. ARS, Zoonot Dis Res Unit, USDA, Natl Anim Dis Ctr, Ames, IA 50010 USA. Anim & Plant Hlth Inspect Serv, USDA, Natl Vet Serv Labs, Ames, IA 50010 USA. Colorado State Univ, Dept Microbiol, Ft Collins, CO 80523 USA. Colorado State Univ, Coll Vet Med & Biomed Sci, Ctr Vet Epidemiol & Anim Dis Surveillance Syst, Ft Collins, CO 80523 USA. Feld Entertainment, Vienna, VA 22182 USA. San Francisco Zool Gardens, San Francisco, CA 94132 USA. Kansas State Univ, Coll Vet Med, Dept Clin Sci, Manhattan, KS 66506 USA. Audubon Ctr Res Endangered Species, New Orleans, LA 70131 USA. RP Peddie, L (reprint author), 15333 Rains Court, Moorpark, CA 93021 USA. NR 44 TC 52 Z9 56 U1 1 U2 12 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 EI 1937-2825 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD MAR PY 2001 VL 32 IS 1 BP 1 EP 16 PG 16 WC Veterinary Sciences SC Veterinary Sciences GA 478LW UT WOS:000171348500001 PM 12790389 ER PT J AU Talley, TS Crooks, JA Levin, LA AF Talley, TS Crooks, JA Levin, LA TI Habitat utilization and alteration by the invasive burrowing isopod, Sphaeroma quoyanum, in California salt marshes SO MARINE BIOLOGY LA English DT Article ID BAY; DEPOSITION; COMMUNITY; ORGANISMS; BENTHOS; CRAB AB In recent years the pace of exotic species introduction and invasion has accelerated, particularly in estuaries and wetlands. Species invasions may affect coastal ecosystems in many ways. Alteration of sedimentary environments, through structure formation and burrowing, has particularly dramatic effects on coastal habitats. This study examines modification of channel bank and marsh edge habitat by the burrowing Australasian isopod Sphaeroma quoyanum Milne Edwards, in created and natural salt marshes of San Diego Bay and San Francisco Bay. Abundance and distribution patterns of this isopod species, its relationships with habitat characteristics, and its effects on sediment properties and bank erosion were examined seasonally, and in several marsh microhabitats. Mean isopod densities were 1541 and 2936 individuals per 0.25 m(2) in San Francisco Bay, and 361 and 1153 individuals per 0.25 m(2) in San Diego Bay study sites during December and July 1998, respectively. This isopod forms dense, anastomosing burrow networks. S. quoyanum densities did not differ as a function of location within creeks or location in natural versus created marshes. Burrows, which are on average 6 mm wide and 2 cm long, were associated with firm sediments containing high detrital biomass. Although erosion is a natural process along salt marsh banks, enclosure experiments demonstrated that isopod activities can enhance sediment loss from banks. In areas infested with S. quoyanum, losses may exceed 100 cm of marsh edge per year. The effects of habitat alteration by this invading species are likely to increase in severity in the coastal zone as these ecosystems become degraded. C1 Univ Calif San Diego, Scripps Inst Oceanog, Marine Life Res Grp, La Jolla, CA 92093 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Levin, LA (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Marine Life Res Grp, La Jolla, CA 92093 USA. NR 59 TC 43 Z9 47 U1 4 U2 17 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD MAR PY 2001 VL 138 IS 3 BP 561 EP 573 DI 10.1007/s002270000472 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 417MG UT WOS:000167838300013 ER PT J AU Artiss, T Schultz, TR Polhemus, DA Simon, C AF Artiss, T Schultz, TR Polhemus, DA Simon, C TI Molecular phylogenetic analysis of the dragonfly genera Libellula, Ladona, and Plathemis (Odonata : Libellulidae) based on mitochondrial cytochrome oxidase I and 16S rRNA sequence data SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID LUCTUOSA BURMEISTER; DNA-SEQUENCE; NUCLEOTIDE-SEQUENCES; SPECIES PHYLOGENIES; EVOLUTIONARY RATES; BEHAVIORAL ECOLOGY; COMBINING DATA; SYSTEMATICS; CONGRUENCE; TREES AB Molecular phylogenetic relationships among members: of the odonate genus Libellula (Odonata: Anisoptera: Libellulidae) were examined using 735 bp of mitochondrial COI and 416 bp of 16S ribosomal RNA gene sequences. Considerable debate exists over several relationships within Libellula, as well over the status of two putative genera often placed as subgenera within Libellula: Ladona and Plathemis. Parsimony and maximum-likelihood analyses of the separate and combined data sets indicate that Plathemis is basal and monophyletic and that Ladona is the sister clade to the remainder of Libellula sensu stricto (s.s.) (all. species within the genus Libellula, excluding Plathemis and Ladona). Moreover, two European taxa, Libellula fulva and L. depressa, were found to occupy a sister group relationship within the Ladona clade. Relationships within Libellula s.s. are less well resolved. However, monophyletic lineages within the genus are largely consistent with morphologically based subgeneric classifications. Although tree topologies from each analysis differed in some details, the differences were in no case statistically significant. The analysis of the combined COI and 16S data yielded trees with overall stronger support than analyses of either gene alone. Several analyses failed to support the monophyly of Libellula sensu late due to the inclusion df one or more outgroup species. However, statistical comparisons of topologies produced by unconstrained analyses and analyses in which the monophyly of Libellula was constrained indicate that any differences are nonsignificant. Based on morphological data, we therefore reject the paraphyly of Libellula and accept the outgroup status of Orthemis ferruginea and Pachydiplax longipennis. (C) 2001 Academic Press. C1 Clark Univ, Dept Biol, Worcester, MA 01610 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. Univ Connecticut, Dept Ecol & Evolut Biol, Storrs, CT 06269 USA. RP Artiss, T (reprint author), Lakeside Sch, 14050 1st Ave NE, Seattle, WA 98125 USA. NR 98 TC 21 Z9 26 U1 3 U2 14 PU ACADEMIC PRESS INC PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAR PY 2001 VL 18 IS 3 BP 348 EP 361 DI 10.1006/mpev.2000.0867 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 411XZ UT WOS:000167526100003 PM 11277629 ER PT J AU Krzywinski, J Wilkerson, RC Besansky, NJ AF Krzywinski, J Wilkerson, RC Besansky, NJ TI Evolution of mitochondrial and ribosomal gene sequences in Anophelinae (Diptera : Culicidae): Implications for phylogeny reconstruction SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE cyt b; ND5; 28S rDNA; evolution; phylogeny; mosquitoes ID DNA-SEQUENCE; SECONDARY STRUCTURE; RNA; SYSTEMATICS; DROSOPHILA; CLASSIFICATION; ORGANIZATION; SUBSTITUTION; PARTITIONS; CHARACTERS AB In this study, two mitochondrial genes, cyt b and ND5, and the D2 expansion segment of the 28S nuclear ribosomal gene were used to reconstruct a phylogeny of the mosquito subfamily Anophelinae. The ingroup consisted of all three genera of Anophelinae and five of six subgenera of Anopheles. Six genera of Culicinae were used as the outgroup. Extreme conservation at the protein level coupled with rapid saturation of synonymous positions probably accounted for the lack of meaningful phylogenetic signal in the cyt b gene. In contrast, abundant variation at all codon positions of the ND5 gene allowed recovery of the basal and most of the recent relationships. Phylogenetic analysis of D2 produced results consistent with those of ND5. Combined analysis indicated well-supported monophyletic Anophelinae (with Chagasia basal), Anopheles + Bironella, and subgeneric clades within the genus Anopheles. Moreover, subgenera Nyssorhynchus and Kerteszia were supported as a monophyletic lineage. The Kishino-Hasegawa test could not reject the monophyly of Anopheles, whereas the recently proposed hypothesis of close affinity of Bironella to the subgenus Anopheles was rejected by the analyses of ND5 and combined data sets. The lack of resolution of Bironella and Anopheles clades, or basal relationships among subgeneric clades within Anopheles, suggests their rapid diversification. Recovery of relationships consistent with morphology and previous molecular studies provides evidence of substantial phylogenetic signal in D2 and ND5 genes at levels of divergence from closely related species to subfamily in mosquitoes. (C) 2001 Academic Press. C1 Univ Notre Dame, Dept Biol Sci, Notre Dame, IN 46556 USA. Smithsonian Inst, Walter Reed Biosystemat Unit, Museum Support Ctr, Washington, DC 20560 USA. RP Krzywinski, J (reprint author), Univ Notre Dame, Dept Biol Sci, Notre Dame, IN 46556 USA. NR 41 TC 51 Z9 57 U1 1 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAR PY 2001 VL 18 IS 3 BP 479 EP 487 DI 10.1006/mpev.2000.0894 PG 9 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 411XZ UT WOS:000167526100013 PM 11277639 ER PT J AU Fox, DW Lewin, WHG Rutledge, RE Morgan, EH Guerriero, R Bildsten, L van der Klis, M van Paradijs, J Moore, CB Dotani, T Asai, K AF Fox, DW Lewin, WHG Rutledge, RE Morgan, EH Guerriero, R Bildsten, L van der Klis, M van Paradijs, J Moore, CB Dotani, T Asai, K TI Search for millisecond periodicities in type I X-ray bursts of the Rapid Burster SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars : individual : Rapid Burster (MXB 1730-335); X-rays : bursts; X-rays : individual : Rapid Burster (MXB 1730-335); X-rays : stars ID TIMING-EXPLORER; COHERENT OSCILLATIONS; EVOLUTION; DISCOVERY AB We have searched the rising portion of type I X-ray bursts observed from the Rapid Burster with the Rossi X-ray Timing Explorer for the presence of periodicities. The 95 per cent confidence upper limit on the average rms variation of near coherent pulsations with a width of less than or similar to1 Hz (in 60-2048 Hz) during the first second of the bursts is <8.8 per cent. We find a possible detection (> 98 per cent significance) at 306.5 Hz. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. US Mil Acad, Dept Phys, W Point, NY 10996 USA. Univ Calif Santa Barbara, Inst Theoret Phys, Santa Barbara, CA 93106 USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Phys, NL-1098 SJ Amsterdam, Netherlands. Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Space & Astronaut Sci, Sagamihara, Kanagawa 229, Japan. RP Fox, DW (reprint author), MIT, Ctr Space Res, Cambridge, MA 02139 USA. NR 30 TC 11 Z9 11 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2001 VL 321 IS 4 BP 776 EP 782 DI 10.1046/j.1365-8711.2001.04085.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 413UG UT WOS:000167629700017 ER PT J AU Volkert, J AF Volkert, J TI Interactive excellence: Defining and developing new standards for the Twenty-first Century SO MUSEUM NEWS LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. RP Volkert, J (reprint author), Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 USA SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD MAR-APR PY 2001 VL 80 IS 2 BP 25 EP + PG 0 WC Art SC Art GA 407PM UT WOS:000167280000022 ER PT J AU Volkert, J AF Volkert, J TI Creativity and beyond: Cultures, values, and change SO MUSEUM NEWS LA English DT Book Review C1 Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. RP Volkert, J (reprint author), Smithsonian Inst, Natl Museum Amer Indian, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 USA SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD MAR-APR PY 2001 VL 80 IS 2 BP 25 EP + PG 0 WC Art SC Art GA 407PM UT WOS:000167280000021 ER PT J AU Faden, RB Alford, MH AF Faden, RB Alford, MH TI A new species of Commelina (Commelinaceae) from Tanzania SO NOVON LA English DT Article DE Commelina; Commelinaceae; Tanzania AB Commelina polhillii Faden &- Alford, a new annual species of Commelina with buff-orange flowers. is described from Tanzania. It differs from the similar C. subulata primarily in seed morphology. However, staminode shape, the presence of basal lobes on the medial anther connective, and differences in spathe pubescence also serve to varying extent to distinguish the two taxa. Leaf anatomy reveals one major difference but primarily helps to unite the two species with a group of approximately seven other species. A preliminary chromosome count. 2n = ca. 30, is recorded. C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20560 USA. Mississippi Coll, Dept Sci Biol, Clinton, MS 39058 USA. RP Faden, RB (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20560 USA. RI Alford, Mac/G-4156-2011 OI Alford, Mac/0000-0002-3448-9735 NR 6 TC 3 Z9 4 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD SPR PY 2001 VL 11 IS 1 BP 16 EP 21 DI 10.2307/3393200 PG 6 WC Plant Sciences SC Plant Sciences GA 429BK UT WOS:000168496000003 ER PT J AU Faden, RB AF Faden, RB TI New taxa of Murdannia (Commelinaceae) from Sri Lanka SO NOVON LA English DT Article DE Commelinaceae; Murdannia; Sri Lanka AB Three new species and three infraspecific taxa of Murdannia are described from Sri Lanka. Murdannia dimorphoides Faden, with subsp. dimorphoides and subsp. perennis Faden, and Murdannia audrevae Faden are endemic to Sri Lanka. Murdannia striatipetala Faden also occurs in southern India. The new variety, Murdannia spirata var, parviflora Faden, is recognized as indigenous in Sri Lanka and naturalized in the southern United States (Florida). Murdannia vaginata var. glabrisepala Faden is described from Sri Lanka, but whether it occurs elsewhere is not firmly established. C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20560 USA. RP Faden, RB (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20560 USA. NR 9 TC 4 Z9 7 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD SPR PY 2001 VL 11 IS 1 BP 22 EP 30 DI 10.2307/3393201 PG 9 WC Plant Sciences SC Plant Sciences GA 429BK UT WOS:000168496000004 ER PT J AU Faden, RB AF Faden, RB TI A new species of Tradescantia (Commelinaceae) from Costa Rica SO NOVON LA English DT Article DE Commelinaceae; Costa Rica; Tradescantia AB A new species of Tradescantia (sect. Cymbispatha), C grantii Faden, is described from Costa Pica. Based on its morphology and karyotype the new species is most closely related to T. plusiantha from Mexico and probably T. deficiens from Mexico and Guatemala. C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20560 USA. RP Faden, RB (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20560 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD SPR PY 2001 VL 11 IS 1 BP 31 EP 35 DI 10.2307/3393202 PG 5 WC Plant Sciences SC Plant Sciences GA 429BK UT WOS:000168496000005 ER PT J AU Ireland, RR AF Ireland, RR TI Buckiella, a new genus in the Hypnaceae (Musci) SO NOVON LA English DT Article DE Buckiella; China; Europe; Hawaiian Islands; Hypnaceae; Musci; New Guinea; North America; Plagiothecium ID MOSSES AB A new genus, Buckiella, is segregated from Plagiothecium. The type species. Buckiella undulata (Hedwig) Ireland, known from western North America, Europe, China, and New Guinea, has plants with strongly undulate leaves, short, inconspicuous triangular leaf decurrencies, minute, granular, cuticular papillae covering the leaf cells, and wrinkled capsules. A second species, B. draytonii (Sullivant) Ireland, endemic to the Hawaiian Islands, with undulate, nondecurrent leaves, cuticular papillae on the leaf cells, and wrinkled capsules is also included in the genus. C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20560 USA. RP Ireland, RR (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20560 USA. NR 18 TC 2 Z9 2 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD SPR PY 2001 VL 11 IS 1 BP 55 EP 62 DI 10.2307/3393208 PG 8 WC Plant Sciences SC Plant Sciences GA 429BK UT WOS:000168496000011 ER PT J AU Wagner, WL Wood, KR Lorence, DH AF Wagner, WL Wood, KR Lorence, DH TI A new species of Cyrtandra (Gesneriaceae) from Kaua'i, Hawaiian Islands SO NOVON LA English DT Article DE Cyrtandra; Gesneriaceae; Hawaiian Islands AB A rare new species of the Pacific genus Cyrtandra, C. paliku, is described from the Hawaiian Islands. It is unique in its combination of thick stems with shaggy, reddish brown villous pubescence, leaves strongly inequilateral, petioles shaggy villous, and calyx weakly zygomorphic and persistent. Known from northeastern Kaua'i, Cyrtandra paliku occurs only on Mount Namahana and is restricted to north-facing rock faces. ii single population of about 70 plants occurs on vertical saturated walls. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. Natl Trop Bot Garden, Kalaheo, HI 96741 USA. RP Wagner, WL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20560 USA. NR 7 TC 2 Z9 3 U1 0 U2 1 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD SPR PY 2001 VL 11 IS 1 BP 146 EP 152 DI 10.2307/3393224 PG 7 WC Plant Sciences SC Plant Sciences GA 429BK UT WOS:000168496000027 ER PT J AU Bobe, R Eck, GG AF Bobe, R Eck, GG TI Responses of African bovids to Pliocene climatic change SO PALEOBIOLOGY LA English DT Article ID EARLY HOMINID EVOLUTION; SIDI HAKOMA TUFF; KOOBI-FORA; HADAR FORMATION; TURKANA BASIN; ETHIOPIA; KENYA; PLIOPLEISTOCENE; MAMMALS; REGION AB The record of fossil mammals from the Shungura Formation, lower Omo Valley of southern Ethiopia, represents one of the largest and most carefully controlled samples for deciphering the responses of land faunas to global-scale climatic change. We use the abundant and continuous fossil record of the family Bovidae to analyze the effects of a late Pliocene climatic shift toward increased aridity in Africa beginning at 2.8 Ma and intensifying at about 2.4 Ma. A database consisting of 4233 specimen-based records collected under well-defined procedures is used to define patterns through time in bovid abundances while also controlling for taphonomic and other potential biases. Univariate and multidimensional (correspondence analysis) methods are used to study changes in bovid abundances through time. Our results indicate that bovids experienced an increase in species richness and a rapid episode of change in taxonomic abundances at 2.8 +/- 0.1 Ma (between Members B and C), and that this shift was followed by gradual and prolonged changes in abundance between 2.8 and 2.0 Ma (between Member C and upper Member G). An analysis of skeletal-element abundances through the Shungura sequence shows that only moderate changes in taphonomic conditions occurred between 3.0 and 2.1 Ma, when the lower Omo Valley was dominated by a large, meandering river, but that significant changes in the mode of preservation accompanied the onset of lacustrine depositional environments at 2.1 Ma (between lower and upper Member G). A juxtaposition of taxonomic with taphonomic patterns shows that the shift in taxonomic abundances at 2.8 Ma occurred in the absence of significant changes in taphonomic conditions. The main changes in bovid relative abundances and diversity appear to have been driven by broad environmental and climatic changes in Africa. As environmental indicators, bovids show a transition in the Omo at about 2.8 Ma from closed and wet environments in Member B to closed but dry environments in Member C. This drying trend intensified in Members D, E, and F, between about 2.5 and 2.3 Ma. In lower Member G, between 2.3 and 2.1 Ma, there was an increase in bovid abundance and diversity, which may be a result of greater environmental heterogeneity. The pattern of environmental change depicted by Shungura bovids is consistent with independently derived evidence of Omo paleoenvironments (from paleosols, paleoflora, and micromammals), and with regional and global evidence of climatic changes, especially acute between 2.8 and 2.3 Ma, that caused the initiation of glacial cycles in the north and drier climate in the tropics of Africa. Even though the Omo bovids showed distinct responses to large-scale climatic and environmental change, the Omo bovid community also had important attributes of long-term stability: two species, Aepyceros shungurae and Tragelaphus nakuae, dominated the community for nearly one million years. This study highlights the importance of carefully controlled collection procedures of fossil vertebrates and provides an important demonstration of the potential complexity in mode and rate of responses of land faunas to climatic change. C1 Smithsonian Inst, Evolut Terr Ecosyst Program, Dept Paleobiol, Washington, DC 20560 USA. Univ Washington, Dept Anthropol, Seattle, WA 98195 USA. RP Bobe, R (reprint author), Smithsonian Inst, Evolut Terr Ecosyst Program, Dept Paleobiol, NHB MRC 121, Washington, DC 20560 USA. OI Bobe, Rene/0000-0001-9059-2203 NR 86 TC 79 Z9 83 U1 0 U2 9 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD SPR PY 2001 VL 27 IS 2 SU S BP 1 EP 47 DI 10.1666/0094-8373(2001)027<0001:ROABTP>2.0.CO;2 PG 47 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 443QG UT WOS:000169351400001 ER PT J AU Richardson, SL AF Richardson, SL TI Endosymbiont change as a key innovation in the adaptive radiation of Soritida (Foraminifera) SO PALEOBIOLOGY LA English DT Review ID PAPUA-NEW-GUINEA; TRIMORPHIC LIFE-CYCLE; LARGER FORAMINIFERA; MARGINOPORA-VERTEBRALIS; BENTHIC FORAMINIFERA; THALASSIA-TESTUDINUM; STABLE ISOTOPES; ALGAL SYMBIOSIS; FLORIDA-KEYS; PHYLOGENY AB A phylogeny of 54 Recent and fossil species of Soritacea (Foraminifera) was used to test the hypothesis that endosymbiosis has driven the evolution of the clade. Endosymbiosis with photosynthetic eukaryotes is the plesiomorphic condition for the entire clade Soritacea. Living species dwell in tropical-subtropical, shallow-water habitats and are characterized by the possession of rhodophyte, chlorophyte, or dinophyte photosymbionts. Two distinct changes in endosymbiont type are recognized when endosymbiont type is mapped in the cladogram of Soritacea: (1) a change from rhodophyte to chlorophyte endosymbionts occurred in the stem lineage of the least inclusive clade containing New clade B, Orbiculinida. and Soritida; and (2) a change from chlorophyte to dinophyte endosymbionts occurred in the stem lineage of the least inclusive clade containing New clade G. New clade H, New clade I, Sorites, Amphisorus, and Orbitolites. When habitat and ontogeny are optimized on the cladogram of Soritida, the acquisition of dinophyte endosymbionts appears as a key innovation that facilitated a switch in habitat from free-living to attached living on non-phytal and phytal substrata. A subsequent change in the attached habitat from nonphytal to predominantly phytal (seagrasses and macroalgae) substrata is accompanied by a peramorphic trend in the megalospheric tests. The diversification (adaptive radiation) of the crown Soritida subclade resulted from the interplay between the acquisition of a key innovation (dinophyte endosymbionts) and the subsequent change in the ecology of the group (radiation to phytal substrates). C1 Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Richardson, SL (reprint author), Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. EM richardson@sms.si.edu NR 166 TC 20 Z9 21 U1 2 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0094-8373 EI 1938-5331 J9 PALEOBIOLOGY JI Paleobiology PD SPR PY 2001 VL 27 IS 2 BP 262 EP 289 DI 10.1666/0094-8373(2001)027<0262:ECAAKI>2.0.CO;2 PG 28 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 441XB UT WOS:000169253900006 ER PT J AU Dziezega, K Griesmann, U Nave, G Bratasz, L AF Dziezega, K Griesmann, U Nave, G Bratasz, L TI Absolute transition rates for transitions from 5p levels in KrII SO PHYSICA SCRIPTA LA English DT Article ID XE-II; COINCIDENCE TECHNIQUE; RADIATIVE LIFETIMES; VACUUM-ULTRAVIOLET; EXCITED-LEVELS; AR-II; NE AB Branching ratios (BR) were measured for 155 electric dipole transitions from 5p and 5p' levels of singly ionized Kr between 200 Mn and 2400 nm. Of these, 83 were measured for the first time. Absolute transition rates for prominent lines, with uncertainties as low as 3% tone standard deviation), were determined with published mean lifetime data for the upper levels. The small uncertainties of our data resolve the discrepancies that were found between several previous measurements. C1 Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. Jagiellonian Univ, Inst Phys, PL-30059 Krakow, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dziezega, K (reprint author), Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. OI Bratasz, Lukasz/0000-0002-5277-2606 NR 24 TC 6 Z9 6 U1 0 U2 1 PU ROYAL SWEDISH ACAD SCIENCES PI STOCKHOLM PA PUBL DEPT BOX 50005, S-104 05 STOCKHOLM, SWEDEN SN 0281-1847 J9 PHYS SCRIPTA JI Phys. Scr. PD MAR PY 2001 VL 63 IS 3 BP 209 EP 218 DI 10.1238/Physica.Regular.063a00209 PG 10 WC Physics, Multidisciplinary SC Physics GA 410UC UT WOS:000167456800006 ER PT J AU Chung, HK Kirby, K Babb, JF AF Chung, HK Kirby, K Babb, JF TI Theoretical study of the absorption spectra of the sodium dimer SO PHYSICAL REVIEW A LA English DT Article ID TRANSITION DIPOLE-MOMENTS; 2 NA ATOMS; SCATTERING LENGTHS; VIBRATIONAL LEVELS; POTENTIAL-BARRIER; BAND SYSTEM; STATE; LIFETIMES; LASER; SPECTROSCOPY AB Absorption of radiation from sodium dimer molecular states correlating to Na(3s)-Na(3s) is investigated theoretically. Vibrational bound and continuum transitions from the singlet X (1)Sigma (+)(g),+ state to the first excited A (1)Sigma (+)(u) and B (1)Pi (u) states and from the triplet a (3)Sigma (+)(u) state to the first excited b (3)Sigma (+)(g) and c (3)Pi (g) states are studied quantum-mechanically. Theoretical and experimental data are used to characterize the molecular properties, taking advantage of knowledge recently obtained from nb initio calculations, spectroscopy, and ultracold atom collision studies. The quantum-mechanical calculations are carried out for temperatures in the range from 1000 to 3000 K, and are compared with previous calculations and measurements where available. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Chung, HK (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. OI Babb, James/0000-0002-3883-9501 NR 55 TC 29 Z9 29 U1 0 U2 8 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAR PY 2001 VL 63 IS 3 AR 032516 DI 10.1103/PhysRevA.63.032516 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 408HP UT WOS:000167321000054 ER PT J AU Jennions, MD Moller, AP Petrie, M AF Jennions, MD Moller, AP Petrie, M TI Sexually selected traits and adult survival: A meta-analysis SO QUARTERLY REVIEW OF BIOLOGY LA English DT Review ID RED-WINGED BLACKBIRDS; LIFETIME REPRODUCTIVE SUCCESS; HISTORY TRADE-OFFS; DAMSELFLY HETAERINA-AMERICANA; PHEASANT PHASIANUS-COLCHICUS; INTENSE NATURAL-SELECTION; SWALLOWS HIRUNDO-RUSTICA; DEPENDENT SEX ORNAMENTS; MALE MATING SUCCESS; GREAT TIT PARUS AB Traits correlated with mak mating success are likely to be subject to sexual selection. Sexually selected characters are thought to be costly to develop and maintain. If males do not vary their investment in sexual traits in relation to their ability to bear the costs, there should be a negative relationship between male longevity or survival and the expression of sexual traits. In particular, a negative relationship is predicted by pureFisherian models for the evolution of sexual ornaments. The same should also be true for traits that evolve via pleiotropy (e.g., due to,sensory exploitation or bias) with no subsequent evolution of condition dependent modification. We collected information on the relationship between traits correlated with male mating rate and estimates of adult male survivorship or life span. In total we obtained 122 samples from 69 studies of 40 species of bird, spider, insect, and fish. In a mete-analysis we calculated the average sample size weighted correlation between trait expression and adult survival Analyses at the level of samples, studies, and species revealed significant positive relationships (r = 0. 08, 0. 10, and 0. 13, respectively; all P < 0.001). The unweighted correlation at the species level was r = 0.24. In general, males with larger ornaments or weapons, greater body size, or higher rates of courtship showed greater survivorship or longevity. This finding is inconsistent with pureFisherian model or other models that do not incorporate condition or quality dependent trait expression. It suggests that male investment in sexually selected traits is not fixed but varies in relation to the ability to pay the underlying costs of expressing these characters. Hence, many secondary sexual characters are likely to be condition dependent In their expression. C1 Smithsonian Trop Res Inst, Unit 0948, Miami, FL 34002 USA. Univ Paris 06, CNRS, URA 258, Ecol Lab, F-75252 Paris 5, France. Univ Newcastle Upon Tyne, Dept Psychol, Evolut & Behav Res Grp, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. RP Jennions, MD (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO AA, Miami, FL 34002 USA. EM MICHAEL.JENNIONS@ANU.EDU.AU; ANDERS.MOLLER@HALL.SNV.JUSSIEU.FR; MARION.PETRIE@NCL.AC.UK RI Jennions, Michael/C-7560-2009 OI Jennions, Michael/0000-0001-9221-2788 NR 200 TC 239 Z9 241 U1 8 U2 118 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0033-5770 J9 Q REV BIOL JI Q. Rev. Biol. PD MAR PY 2001 VL 76 IS 1 BP 3 EP 36 DI 10.1086/393743 PG 34 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 414LJ UT WOS:000167667900001 PM 11291569 ER PT J AU Guzman, HM Guevara, CA AF Guzman, HM Guevara, CA TI Coral reefs of Bocas del Toro, Panama: IV. Distribution, structure and conservation status of continental reefs in Valiente Peninsula SO REVISTA DE BIOLOGIA TROPICAL LA Spanish DT Article DE coral reefs; Panama; Bocas del Toro; Acropora; biodiversity; marine conservation ID DIVERSITY; PATTERNS; ISLANDS; FLORIDA AB This is the fourth and last contribution describing the individual structure, distribution and conservation status of coral reefs in the Province of Bocas del Toro. Here we describe 14 new reefs along 129 km of coast from Peninsula Valiente to Rio Calovebora. Average live coral coverage for this region was 17.1% (+/-3.6%), mainly in the western region of the peninsula (Bahia Bluefield and Ensenada Tobobe). Coral cover increases with depth (> 5 m) for most species at several reefs and the corals Porites furcata and Acropora palmata dominated shallow waters. Acropora palmata was found abundant in 43% of the studied reefs and toward the regions of the Ensenada Tobobe and Punta Valiente. Coral recruitment rates were similar in distribution to those reefs with greater coral coverage, with average densities of 4 recruit/m(2) (maximum 9 recruits/m(2)) and mainly Agaricia spp., Porites astreoides and Siderastrea siderea. The greater diversity of corals and sponges was recorded toward the western side of the peninsula, with a total of 55 coral species in the study area, including two new records for Bocas del Toro (59 species in total), Dichocoenia stellaris and Madracis luciphila and increasing the diversity of corals of Panama to 65 species. We found 24 species of octocorals and Gorgonia mariae, Muriceopsis sulphurea and Muricea laxaoosens, are informed for the first time to the area, increasing in 10% the diversity for Bocas del Toro (32 in total). We recorded 48 sponges, including five new species for the area and representing an increase of 9% in the total number (58). Large populations of Acropora palmata were found in the Ensenada Tobobe, what justifies once again the need for modifying the existing protected area, so that this new region is incorporated within the conservation plans. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. NR 19 TC 15 Z9 16 U1 1 U2 9 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, COSTA RICA SN 0034-7744 J9 REV BIOL TROP JI Rev. Biol. Trop. PD MAR PY 2001 VL 49 IS 1 BP 53 EP 66 PG 14 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 494YE UT WOS:000172312800006 PM 11795170 ER PT J AU Sadler, PM Tai, RH AF Sadler, PM Tai, RH TI Success in introductory college physics: The role of high school preparation SO SCIENCE EDUCATION LA English DT Article ID STUDENTS; CHEMISTRY; PERCEPTIONS AB High school teachers and college physics professors differ in their beliefs concerning the extent to which a high school physics course prepares students for college physics success. In this study of 1,933 introductory college physics students, demographic and schooling factors account for a large fraction of the variation in college physics grades at 18 colleges and universities from around the nation. Controlling for student backgrounds, taking a high school physics course has a modestly positive relationship with the,grade earned in introductory college physics. More rigorous preparation, including calculus and 2 years of high school physics, predicts higher grades. Students who had high school courses that spent more time on fewer topics, concepts, problems, and labs performed much better in college than those who raced through more content in a textbook-centered course. College professors should recognize that a substantial fraction of the variation observed in the performance of students they teach can be explained by the range in effectiveness of their pre-college preparation, not simply innate ability. Although students without a high school physics course often do well in college physics, they are more likely to be academically stronger, with more educated parents, having previously taken calculus, and taking physics in their sophomore or junior year in college. (C) 2001 John Wiley & Sons, Inc. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Grad Sch Educ, Cambridge, MA 02138 USA. CUNY, Coll Staten Isl, New York, NY 10021 USA. RP Sadler, PM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 66 TC 45 Z9 47 U1 1 U2 6 PU JOHN WILEY & SONS INC PI NEW YORK PA 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0036-8326 J9 SCI EDUC JI Sci. Educ. PD MAR PY 2001 VL 85 IS 2 BP 111 EP 136 PG 26 WC Education & Educational Research SC Education & Educational Research GA 401YC UT WOS:000166955800002 ER PT J AU Funk, VA AF Funk, VA TI SSZ 1970-1989: A view of the years of conflict SO SYSTEMATIC BIOLOGY LA English DT Editorial Material C1 Smithsonian Inst, NHB 166, US Natl Herbarium, Washington, DC 20560 USA. RP Funk, VA (reprint author), Smithsonian Inst, NHB 166, US Natl Herbarium, Washington, DC 20560 USA. NR 16 TC 2 Z9 2 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI LONDON PA 11 NEW FETTER LANE, LONDON EC4P 4EE, ENGLAND SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD MAR-APR PY 2001 VL 50 IS 2 BP 153 EP 155 DI 10.1080/10635150151125798 PG 3 WC Evolutionary Biology SC Evolutionary Biology GA 431XN UT WOS:000168657200001 PM 12116925 ER PT J AU Seitel, P AF Seitel, P TI Collecting folklore in Mauritius SO WESTERN FOLKLORE LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Seitel, P (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CALIF FOLKLORE SOC PI POMONA PA WESTERN FOLKLORE DEPT OF ENGL/FOREIGN LANGUAGES 3801 W.TEMPLE AVENUE, POMONA, CA 91768-4010 USA SN 0043-373X J9 WESTERN FOLKLORE JI West. Folk. PD SPR-SUM PY 2001 VL 60 IS 2-3 BP 237 EP 238 DI 10.2307/1500381 PG 2 WC Folklore SC Arts & Humanities - Other Topics GA 601FA UT WOS:000178434800011 ER PT J AU De, SR Heaney, PJ Vicenzi, EP Wang, JH AF De, SR Heaney, PJ Vicenzi, EP Wang, JH TI Chemical heterogeneity in carbonado, an enigmatic polycrystalline diamond SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE carbonado; C-13/C-12; secondary ion mass spectroscopy; cathodoluminescence; nitrogen ID CHICXULUB CRATER; SILICON-CARBIDE; IMPACT CRATER; MELT ROCK; ORIGIN; CATHODOLUMINESCENCE; AGGREGATION; DIFFUSION; DEFECTS; GROWTH AB Carbonade, a polycrystalline variety of diamond, is characterized by unusual carbon isotope compositions with bulk delta C-13 values clustered tightly between -23 and -30 parts per thousand (relative to PDB). These values are significantly lighter than harzburgitic diamond (with a range in delta C-13 from -1 to -10 parts per thousand) and fall near the lower extreme for eclogitic diamond (ranging from +3 to -34 parts per thousand). In combination with textural and inclusion data, these isotopic compositions have led scientists to question whether carbonade originated in the mantle or in the crust. Previous studies of carbonade have revealed a bimodal grain size distribution that correlates with cathodoluminescence (CL) emissions. We believe that these textures result from a two-step growth process, and we have obtained additional chemical evidence that supports the identification of two distinct crystal populations. Ion microprobe analyses of a Central African carbonade reveal a bimodal distribution of delta C-13 values of -24 and -26 parts per thousand (with an instrumental precision of +/- 0.29 parts per thousand). Secondary ion mass spectrometry analyses also demonstrate that this delta C-13 distribution coincides with variations in nitrogen abundance, and both of these chemical zonations correlate with CL emission signatures. A one-dimensional analysis of self-diffusion of carbon in diamond suggests that isotopic homogenization occurs extremely slowly, even under upper mantle conditions. Whereas the microscale distribution of carbon isotopes in carbonade does not constrain the temperature, pressure or time of carbonade formation, it does provide a geochemical signature that recorded the dynamics of the growth process. (C) 2001 Elsevier Science B.V. All rights reserved. C1 Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Mineral Sci, Washington, DC 20560 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. RP De, SR (reprint author), NASA, Ames Res Ctr, Exobiol Branch, MS-239-4, Moffett Field, CA 94035 USA. RI Wang, Jianhua/D-6500-2011 OI Wang, Jianhua/0000-0002-7671-2413 NR 67 TC 24 Z9 25 U1 2 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD FEB 28 PY 2001 VL 185 IS 3-4 BP 315 EP 330 DI 10.1016/S0012-821X(00)00369-1 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 405WC UT WOS:000167182700006 ER PT J AU Tuthill, PG Monnier, JD Danchi, WC AF Tuthill, PG Monnier, JD Danchi, WC TI A dusty torus around the luminous young star LkH alpha 101 SO NATURE LA English DT Article ID HERBIG AE/BE STARS; INTERMEDIATE-MASS STARS; PROTOSTELLAR DISKS; INFRARED-EMISSION; STELLAR OBJECTS; PHOTOEVAPORATION AB A star forms when a cloud of dust and gas collapses. It is generally believed that this collapse first produces a flattened rotating disk(1,2), through which matter is fed onto the embryonic star at the centre of the disk. When the temperature and density at the centre of the star pass a critical threshold, thermonuclear fusion begins. The remaining disk, which can still contain up to 0.3 times the mass of the star(3-5), is then sculpted and eventually dissipated by the radiation and wind from the newborn star. But this picture of the structure and evolution of the disk remains speculative because of the lack of morphological data of sufficient resolution and uncertainties regarding the underlying physical processes. Here we present images of a young star, LkH alpha 101, in which the structure of the inner accretion disk is resolved. We rnd that the disk is almost face-on, with a central gap (or cavity) and a hot inner edge. The cavity is bigger than previous theoretical predictions(6), and we infer that the position of the inner edge is probably determined by sublimation of dust grains by direct stellar radiation, rather than by disk-reprocessing or viscous-heating processes as usually assumed(29). C1 Univ Sydney, Sch Phys, Dept Astron, Sydney, NSW 2006, Australia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tuthill, PG (reprint author), Univ Sydney, Sch Phys, Dept Astron, Sydney, NSW 2006, Australia. NR 29 TC 91 Z9 93 U1 0 U2 0 PU MACMILLAN PUBLISHERS LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 22 PY 2001 VL 409 IS 6823 BP 1012 EP 1014 DI 10.1038/35059014 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 405FT UT WOS:000167148800036 PM 11234003 ER PT J AU Mitrovica, JX Tamisiea, ME Davis, JL Milne, GA AF Mitrovica, JX Tamisiea, ME Davis, JL Milne, GA TI Recent mass balance of polar ice sheets inferred from patterns of global sea-level change SO NATURE LA English DT Article ID GLACIAL ISOSTATIC-ADJUSTMENT; TRENDS; FIELD; RISE AB Global sea level is an indicator of climate change(1-3), as it is sensitive to both thermal expansion of the oceans and a reduction of land-based glaciers. Global sea-level rise has been estimated by correcting observations from tide gauges for glacial isostatic adjustment-the continuing sea-level response due to melting of Late Pleistocene ice-and by computing the global mean of these residual trends(4-9). In such analyses, spatial patterns of sealevel rise are assumed to be signals that will average out over geographically distributed tide-gauge data. But a long history of modelling studies(10-12) has demonstrated that non-uniform- that is, non-eustatic-sea-level redistributions can be produced by variations in the volume of the polar ice sheets. Here we present numerical predictions of gravitationally consistent patterns of sea-level change following variations in either the Antarctic or Greenland ice sheets or the melting of a suite of small mountain glaciers. These predictions are characterized by geometrically distinct patterns that reconcile spatial variations in previously published sea-level records. Under the-albeit coarse-assumption of a globally uniform thermal expansion of the oceans, our approach suggests melting of the Greenland ice complex over the last century equivalent to similar to0.6 mm yr(-1) of sea-level rise. C1 Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Durham, Dept Geol Sci, Sci Labs, Durham DH1 3LE, England. RP Mitrovica, JX (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada. RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 29 TC 249 Z9 257 U1 9 U2 61 PU MACMILLAN PUBLISHERS LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 22 PY 2001 VL 409 IS 6823 BP 1026 EP 1029 DI 10.1038/35059054 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 405FT UT WOS:000167148800041 PM 11234008 ER PT J AU Kaaret, P Prestwich, AH Zezas, A Murray, SS Kim, DW Kilgard, RE Schlegel, EA Ward, MJ AF Kaaret, P Prestwich, AH Zezas, A Murray, SS Kim, DW Kilgard, RE Schlegel, EA Ward, MJ TI Chandra High-Resolution Camera observations of the luminous X-ray source in the starburst galaxy M82 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; galaxies : individual : M82; galaxies : starburst; galaxies : stellar content; X-rays : galaxies ID ACTIVE GALACTIC NUCLEUS; STAR-CLUSTERS; VELOCITY DISPERSION; SUPERNOVA-REMNANTS; RADIO OBSERVATIONS; ROSAT OBSERVATIONS; BLACK-HOLES; PERFORMANCE; CALIBRATION; DISCOVERY AB We analyse Chandra High Resolution Camera observations of the starburst galaxy M82, concentrating on the most luminous X-ray source. We find a position for the source of RA = O9(h)55(m)50.(s)2, Dec. = +69 degrees 40'46."7 (J2000) with a 1 sigma radial error of 0.7 arcsec. The accurate X-ray position shows that the luminous source is neither at the dynamical centre of M82 nor coincident with any suggested radio AGN candidate. The source is highly variable between observations, which suggests that it is a compact object and not a supernova or remnant. There is no significant short-term variability within the observations. Dynamical friction and the off-centre position place an upper bound of 10(5)-10(6) M-. on the mass of the object, depending on its age. The X-ray luminosity suggests a compact object mass of at least 500 M-.. Thus the luminous source in M82 may represent a new class of compact object with a mass intermediate between those of stellar-mass black hole candidates and supermassive black holes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Kaaret, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 43 TC 182 Z9 184 U1 0 U2 1 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 21 PY 2001 VL 321 IS 2 BP L29 EP L32 DI 10.1046/j.1365-8711.2001.04064.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 503PP UT WOS:000172807100001 ER PT J AU Machacek, ME Bryan, GL Abel, T AF Machacek, ME Bryan, GL Abel, T TI Simulations of pregalactic structure formation with radiative feedback SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : formation; hydrodynamics; methods : numerical ID ADAPTIVE MESH REFINEMENT; 1ST COSMOLOGICAL OBJECTS; POPULATION-III OBJECTS; GALACTIC GAS CLOUDS; X-RAY-CLUSTERS; HYDROGEN MOLECULES; INTERGALACTIC MEDIUM; EARLY UNIVERSE; STAR-FORMATION; HIGH-REDSHIFT AB We present results from three-dimensional hydrodynamic simulations of the high-redshift collapse of pregalactic clouds including feedback effects from a soft H(2) photodissociating UV radiation field. The simulations use an Eulerian adaptive mesh refinement technique to follow the nonequilibrium chemistry of nine chemical species with cosmological initial conditions drawn from a popular Lambda -dominated cold dark matter model. The results confirm that the soft UV background can delay the cooling and collapse of small halos (similar to 10(6) M.). For reasonable values of the photodissociating flux, the H(2) fraction is in equilibrium throughout most of the objects we simulate. We determine the mass threshold for collapse for a range of soft-UV fluxes and also derive a simple analytic expression. Continuing the simulations beyond the point of initial collapse demonstrates that the fraction of gas which can cool depends mostly on the virial mass of the halo and the amount of soft-UV flux, with remarkably little scatter. We parameterize this relation, for use in semianalytic models. C1 Northeastern Univ, Dept Phys, Boston, MA 02115 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Machacek, ME (reprint author), Northeastern Univ, Dept Phys, Boston, MA 02115 USA. NR 63 TC 218 Z9 218 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2001 VL 548 IS 2 BP 509 EP 521 DI 10.1086/319014 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406FU UT WOS:000167204900001 ER PT J AU Cappi, M Mazzotta, P Elvis, M Burke, DJ Comastri, A Fiore, F Forman, W Fruscione, A Green, P Harris, D Hooper, EJ Jones, C Kaastra, JS Kellogg, E Murray, S McNamara, B Nicastro, F Ponman, TJ Schlegel, EM Siemiginowska, A Tananbaum, H Vikhlinin, A Virani, S Wilkes, B AF Cappi, M Mazzotta, P Elvis, M Burke, DJ Comastri, A Fiore, F Forman, W Fruscione, A Green, P Harris, D Hooper, EJ Jones, C Kaastra, JS Kellogg, E Murray, S McNamara, B Nicastro, F Ponman, TJ Schlegel, EM Siemiginowska, A Tananbaum, H Vikhlinin, A Virani, S Wilkes, B TI Chandra study of an overdensity of X-ray sources around two distant (z similar to 0.5) clusters SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : clusters : general; X-rays : galaxies; X-rays : general ID ROSAT SERENDIPITY SURVEY; ACTIVE GALACTIC NUCLEI; LARGE-SCALE STRUCTURE; GALAXY CLUSTERS; ANGULAR-CORRELATION; STARBURST GALAXIES; RICH CLUSTERS; LOCKMAN FIELD; DEEP SURVEY; COUNTS AB We present results from a Chandra X-Ray Observatory study of the field X-ray source populations in four different observations: two high-redshift (z similar to 0.5) clusters of galaxies 3C 295 and RX J003033.2+261819; and two noncluster fields with similar exposure time. Surprisingly, the 0.5-2 keV source surface densities (similar to 900-1200 sources deg(-2) at a flux limit of 1.5 x 10(-15) ergs cm(-2) s(-1)) measured in an similar to 8' x 8' area surrounding each cluster exceed by a factor of similar to2 the value expected on the basis of the ROSAT and Chandra log N-log S, with a significance of similar to 2 sigma each, or similar to 3.5 sigma when the two fields are combined (i.e., a probability to be a statistical fluctuation of < 1% and < 0.04%, respectively). The same analysis performed on the noncluster fields and on the outer chips of the cluster fields does not show evidence of such an excess. In both cluster fields, the summed 0.5-10 keV spectrum of the detected objects is well fitted by a power law with Gamma similar to 1.7 similar to active galactic nuclei (AGNs) and shows no sign of intrinsic absorption. The few (similar to 10 of 35) optical identifications available to date confirm that most of them are, as expected, AGNs, but the number of redshifts available is too small to allow conclusions on their nature. We discuss possible interpretations of the overdensity in terms of a statistical variation of cosmic background sources; a concentration of AGNs and/or powerful starburst galaxies associated with the clusters; and gravitational lensing of background QSOs by the galaxy clusters. All explanations, however, are difficult to reconcile with the large number of excess sources detected. Deeper X-ray observations and more redshifts measurements are clearly required to settle the issue. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CNR, Ist TeSRE, I-40131 Bologna, Italy. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Osservatorio Astron Bologna, I-40127 Bologna, Italy. Osservatorio Astron Roma, I-00044 Frascati, Italy. SRON, NL-3584 CA Utrecht, Netherlands. Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP Cappi, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Cappi, Massimo/F-4813-2015; Comastri, Andrea/O-9543-2015; Mazzotta, Pasquale/B-1225-2016; OI Comastri, Andrea/0000-0003-3451-9970; Mazzotta, Pasquale/0000-0002-5411-1748; Cappi, Massimo/0000-0001-6966-8920; Nicastro, Fabrizio/0000-0002-6896-1364; Wilkes, Belinda/0000-0003-1809-2364; Forman, William/0000-0002-9478-1682 NR 71 TC 59 Z9 59 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2001 VL 548 IS 2 BP 624 EP 638 DI 10.1086/318998 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406FU UT WOS:000167204900010 ER PT J AU Elmegreen, BG Kim, S Staveley-Smith, L AF Elmegreen, BG Kim, S Staveley-Smith, L TI A fractal analysis of the HI emission from the Large Magellanic Cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : ISM; ISM : clouds; ISM : structure; Magellanic Clouds; turbulence ID NEUTRAL INTERSTELLAR-MEDIUM; NEARBY DWARF GALAXIES; POWER SPECTRUM; HIERARCHICAL STRUCTURE; IRREGULAR GALAXIES; MOLECULAR CLOUDS; STAR-FORMATION; SIMULATIONS; TURBULENCE; SCALE AB Fourier transform power spectra of the distribution of neutral hydrogen emission in the Large Magellanic Cloud is approximately a power law over similar to 2 decades in length. Power spectra in the azimuthal direction look about the same as the rectilinear spectra. No difference is seen between power spectra of single-channel maps and power spectra of either the peak emission map or the integrated emission map at the same location. There is a slight steepening of the average one-dimensional and two-dimensional LMC power spectra at high spatial frequencies. Delta-variance methods also show the same power-law structure. These results suggest that most of the interstellar medium in the LMC is fractal, presumably the result of pervasive turbulence, self-gravity, and self-similar stirring. The similarity between the channel and integrated maps suggests they cover about the same line-of-sight depth. The slight steepening of the power spectra at high spatial frequency, corresponding to wavelengths smaller than similar to 100 pc, could mark the transition from large-scale emission that is relatively shallow on the line of sight to small-scale emission that is relatively thick on the line of sight. Such a transition, if real, would provide a method to obtain the thickness of a face-on galactic gas layer. To check this possibility, three-dimensional fractal models are made from the inverse Fourier transform of noise with a power-law cutoff. The models are viewed in projection with a Gaussian density distribution on the line of sight to represent a face-on galaxy disk with finite disk thickness. The density structure from turbulence is simulated in the models by using a log-normal density distribution function with a scale factor dependent on the Mach number. Additional density structure from simulated H I phase transitions is included in some models. After tuning the Mach number, galaxy thickness, and mathematical form of the phase transition, the models can be made to reproduce the observed LMC power spectra, the amplitude of the H I brightness fluctuations, and the probability distribution function for brightness. In all cases, the H I structure arises from a relatively thin layer in the LMC; the thick part of the H I disk has little spatial structure. The large amplitude of the observed intensity variations cannot be achieved by turbulence alone; phase transitions are required. The character of the fractal H I structure in the LMC is viewed in another way by comparing positive and negative images of the integrated emission. For the isotropic fractal models, these two images have the same general appearance, but for the LMC they differ markedly. The H I is much more filamentary in the LMC than in an isotropic fractal, making the geometric structure of the high-emission regions qualitatively different than the geometric structure of the low-emission (intercloud) regions. The high-emission regions are also more sharply peaked than the low-emission regions, suggesting that compressive events formed the high-emission regions, and expansion events, whether from explosions or turbulence, formed the low-emission regions. The character of the structure is also investigated as a function of scale using unsharp masks and enlargements with four different resolutions. The circular quality of the low-emission regions and the filamentary quality of the high-emission regions is preserved on scales ranging from several tens to several hundreds of parsecs. The spatial scales for sources of turbulent energy input may be illustrated by rms variations in the power spectra with position in the galaxy. This rms decreases from similar to 0.6 at kpc scales to similar to 0.25 on similar to 20 pc scales. The large-scale variations are probably from known supershells. The smaller scale variations could be the result of a combination of turbulent cascades from these large-scale energy inputs and additional energy sources with smaller sizes. C1 IBM Corp, Div Res, TJ Watson Res Ctr, Yorktown Hts, NY 10598 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Elmegreen, BG (reprint author), IBM Corp, Div Res, TJ Watson Res Ctr, POB 218, Yorktown Hts, NY 10598 USA. EM bge@watson.ibm.com; skim@cfa.harvard.edu; lstavele@atnf.csiro.au RI Staveley-Smith, Lister/A-1683-2011 OI Staveley-Smith, Lister/0000-0002-8057-0294 NR 46 TC 116 Z9 118 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2001 VL 548 IS 2 BP 749 EP 769 DI 10.1086/319021 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406FU UT WOS:000167204900019 ER PT J AU Chakrabarty, D Pivovaroff, MJ Hernquist, LE Heyl, JS Narayan, R AF Chakrabarty, D Pivovaroff, MJ Hernquist, LE Heyl, JS Narayan, R TI The central X-ray point source in Cassiopeia A SO ASTROPHYSICAL JOURNAL LA English DT Review DE accretion, accretion disks; black hole physics; stars : neutron; supernovae : individual (Cassiopeia A); supernova remnants; X-rays : stars ID SUPERNOVA REMNANT CASSIOPEIA; SOFT GAMMA-REPEATER; ULTRAMAGNETIZED NEUTRON-STAR; LARGE-MAGELLANIC-CLOUD; RESOLUTION CAMERA HRC; BLACK-HOLE; RADIO-QUIET; RCW 103; SURFACE-TEMPERATURE; MODEL ATMOSPHERES AB The spectacular "first light" observation by the Chandra X-Ray Observatory revealed an X-ray point source near the center of the 300 yr old Cas A supernova remnant. We present an analysis of the public X-ray spectral and timing data. No coherent pulsations were detected in the Chandra/HRC data. The 3 sigma upper limit on the pulsed fraction is less than 35% for P > 20 ms. The Chandra/ACIS spectrum of the point source may be fitted with an ideal blackbody (kT = 0.5 keV) or with blackbody models modified by the presence of a neutron star atmosphere (kT = 0.25-0.35 keV), but the temperature is higher and the inferred emitting area lower than expected for a 300 yr old neutron star according to standard cooling models. The spectrum may also be fitted with a power-law model (photon index Gamma = 2.8-3.6). Both the spectral properties and the timing limits of the point source are inconsistent with a young Crab-like pulsar but are quite similar to the properties of the anomalous X-ray pulsars. The spectral parameters are also very similar to those of the other radio-quiet X-ray point sources in the supernova remnants Pup A, RCW 103, and PKS 1209-52. Current limits on an optical counterpart for the Cas A point source rule out models that invoke fallback accretion onto a compact object if fallback disk properties are similar to those in quiescent low-mass X-ray binaries. However, the optical limits are marginally consistent with plausible alternative assumptions for a fallback disk. In this case, accreting neutron star models can explain the X-ray data, but an accreting black hole model is not promising. C1 MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chakrabarty, D (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM deepto@space.mit.edu; mjp@space.mit.edu; lhernqui@kona.harvard.edu; jheyl@cfa.harvard.edu; rnarayan@cfa.harvard.edu RI Pivovaroff, Michael/M-7998-2014; OI Pivovaroff, Michael/0000-0001-6780-6816; Narayan, Ramesh/0000-0002-1919-2730 NR 137 TC 82 Z9 82 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2001 VL 548 IS 2 BP 800 EP 810 DI 10.1086/318994 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406FU UT WOS:000167204900022 ER PT J AU Slane, P Hughes, JP Edgar, RJ Plucinsky, PP Miyata, E Tsunemi, H Aschenbach, B AF Slane, P Hughes, JP Edgar, RJ Plucinsky, PP Miyata, E Tsunemi, H Aschenbach, B TI RX J0852.0-4622: Another nonthermal shell-type supernova remnant (G266.2-1.2) SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (G266.2-1.2); radiation mechanisms : nonthermal; supernova remnants; X-rays : ISM ID X-RAY-EMISSION; SHOCK ACCELERATION; DISCOVERY; VELA; J1713.7-3946; ELECTRONS; SN-1006; TI-44 AB The newly discovered supernova remnant G266.2-1.2 (RX J0852.0-4622), along the line of sight to the Vela supernova remnant (SNR), was observed with ASCA for 120 ks. We find that the X-ray spectrum is featureless and well described by a power law, extending to three of the class of shell-type SNRs dominated by nonthermal X-ray emission. Like G347.3-0.5, this low-latitude remnant displays discrete regions of enhanced emission along the rim as well as faint nonthermal emission from the interior. We derive limits on the thermal content of the remnant emission, although the presence of the Vela SNR compromises our ability to seriously constrain a low-temperature component. Limits placed on the amount of Sc-K emission are compared with the expected flux based on the reported Ti-44 emission from G266.2-1.2. We also report on an unresolved X-ray source surrounded by diffuse emission near the center of the remnant. The properties of the source are not well determined but appear consistent with the interpretation that the source is a neutron star surrounded by a synchrotron nebula. Alternatively, the source may be associated with one of two stars located within the positional error circle, but this appears somewhat unlikely. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. Japan Sci & Technol Corp, CREST, Tsukuba, Ibaraki 3050047, Japan. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 26 TC 134 Z9 136 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2001 VL 548 IS 2 BP 814 EP 819 DI 10.1086/319033 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406FU UT WOS:000167204900024 ER PT J AU Ueta, T Meixner, M Dayal, A Deutsch, LK Fazio, GG Hora, JL Hoffmann, WF AF Ueta, T Meixner, M Dayal, A Deutsch, LK Fazio, GG Hora, JL Hoffmann, WF TI Discovery of an extended dust emission around IRAS 18576+0341 (AFGL 2298) at 10.3 and 18.0 microns: A new luminous blue variable candidate? SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust, extinction; infrared : stars; stars : individual (IRAS 18576+0341, AFGL 2298); stars : mass loss ID PROTOPLANETARY NEBULA CANDIDATES; ETA-CARINAE; PLANETARY-NEBULAE; CIRCUMSTELLAR ENVELOPES; MASER EMISSION; STARS; SPECTRA; SPECTROMETER; PHOTOMETRY; MORPHOLOGY AB We report the detection of extended mid-infrared emission from IRAS 18576+0341 (AFGL 2298). The object shows a dusty circumstellar shell that has diameter of greater than or similar to 7" at 10.3 and 18.0 mum. The dust nebula shows two emission peaks concentrically elongated and symmetrically oriented on the opposite sides of the third, central peak, which appears to be the central star of the system. The observed mid-infrared morphology indicates that the circumstellar dust shell has an equatorially enhanced material distribution, which is a common signature of stellar objects that have experienced mass loss. Radiative transfer model calculations suggest that the central star is an extremely bright star at a distance (L-* = 10(6.4) L .) of about 10 kpc: this object is best described as a new luminous blue variable candidate. The circumstellar dust shell seems to have been generated by an equatorially-enhanced mass loss process with (M) over dot greater than or equal to 6.8 x 10(-6) M. yr(-1) and (M) over dot (pole)/(M) over dot (eq) similar to 0.5. C1 Univ Illinois, Dept Astron, Urbana, IL 61801 USA. CALTECH, Jet Prop Lab, IPAC, Pasadena, CA 91125 USA. Boston Univ, Dept Astron, Boston, MA 02215 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Ueta, T (reprint author), Univ Illinois, Dept Astron, MC-221, Urbana, IL 61801 USA. OI Hora, Joseph/0000-0002-5599-4650 NR 56 TC 23 Z9 23 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2001 VL 548 IS 2 BP 1020 EP 1028 DI 10.1086/319004 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406FU UT WOS:000167204900042 ER PT J AU DeLuca, EE Hurlburt, NE AF DeLuca, EE Hurlburt, NE TI Magnetic diffusion in stratified atmospheres SO ASTROPHYSICAL JOURNAL LA English DT Article DE convection; MHD; stars : interiors; Sun : magnetic fields ID TURBULENT TRANSPORT; FIELD; POINT AB The predictions from mean field electrodynamics have been questioned because of the strong feedback of small-scale magnetic structure on the velocity fields. In two dimensions, this nonlinear feedback results in a lengthening of the turbulent decay time. In three dimensions a-quenching is predicted. Previous studies assumed a homogeneous fluid. We will present recent results from two-dimensional compressible MHD decay simulations in a highly stratified atmosphere that more closely resembles the solar convection zone. Our results show that the field geometry has a strong influence on the decay rate : vertical fields remain fairly constant for a period of time and then rapidly decay on the turbulent timescale; horizontal fields decay at an intermediate rate with strong fields persisting near the top and bottom boundaries. The implication of our results for understanding solar active region decay is discussed. C1 Harvard Smithsonian Ctr Astrophys, Harvard Smithsonian Observ, Cambridge, MA 02138 USA. Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA. RP DeLuca, EE (reprint author), Harvard Smithsonian Ctr Astrophys, Harvard Smithsonian Observ, 60 Garden St,MS 58, Cambridge, MA 02138 USA. RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 NR 10 TC 6 Z9 6 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2001 VL 548 IS 2 BP 1093 EP 1101 DI 10.1086/318995 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406FU UT WOS:000167204900048 ER PT J AU Nisenson, P Papaliolios, C AF Nisenson, P Papaliolios, C TI Detection of earth-like planets using apodized telescopes SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation : interferometers; planetary systems; stars : imaging; techniques : interferometric ID INTERFEROMETRIC ARRAYS AB The mission of NASA's Terrestrial Planet Finder (TPF) is to find Earth-like planets orbiting other stars and characterize the atmospheres of these planets using spectroscopy. Because of the enormous brightness ratio between the star and the reflected light from the planet, techniques must be found to reduce the brightness of the star. The current favorite approach to doing this is with interferometry: interfering the light from two or more separated telescopes with a pi phase shift, nulling out the starlight. While this technique can, in principle, achieve the required dynamic range, building a space interferometer that has the necessary characteristics poses immense technical difficulties. In this paper, we suggest a much simpler approach to achieving the required dynamic range. By simply adjusting the transmissive shape of a telescope aperture, the intensity in large regions around the stellar image can be reduced nearly to zero. This approach could lead to construction of a TPF using conventional technologies, requiring space optics on a much smaller scale than the current TPF approach. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Nisenson, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 13 TC 132 Z9 132 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2001 VL 548 IS 2 BP L201 EP L205 DI 10.1086/319110 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 406HD UT WOS:000167208100021 ER PT J AU Morris, MR de Queiroz, K Morizot, DC AF Morris, MR de Queiroz, K Morizot, DC TI Phylogenetic relationships among populations of northern swordtails (Xiphophorus) as inferred from allozyme data SO COPEIA LA English DT Article ID GENUS XIPHOPHORUS; POLYMORPHIC CHARACTERS; EVOLUTIONARY TREES; ENZYME LOCI; FISHES; POECILIIDAE; SYSTEMATICS; SEQUENCES; PARSIMONY; INFERENCE AB Twenty-nine populations of Xiphophorus fishes representing nine species of northern swordtails, one southern swordtail and a platyfish were assayed electrophoretically for allozyme variation. Phylogenetic relationships were inferred using parsimony and likelihood analysis of gene frequency characters, as well as Fitch-Margoliash, minimum evolution and neighbor-joining analyses of genetic distances. The phylogenetic relationships among species that were well supported in all analyses included (1) monophyly of the northern swordtails, (2) the pygmaeus clade of Xiphophorus nigrensis, X. multilineatus, and X. pygmaeus, and (3) the dade of X. nigrensis and X. multilineatus. Of those species represented by more than one population, all analyses supported monophyly of X. montezumae and weakly supported monophyly of X. nezahualcoyotl and X, birchmanni. only the distance analyses supported monophyly of X cortezi, and the support was weak. Finally, all analyses supported a clade including X. nezahualcoyotl from the Rio Tamesi drainage and some populations from the Rio Panuco drainage, that is, nonmonophyly of the set of populations from the Rio Panuco drainage. Previously published trees based on morphology, behavior and randomly amplified DNAs were generally congruent with the optimal trees for the allozyme data and were not rejected by those data; in contrast, trees based on DNA sequences were more incongruent with the optimal trees for the allozyme data and were rejected by those data. C1 Ohio Univ, Dept Biol Sci, Athens, OH 45701 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. Univ Texas, MD Anderson Canc Ctr, Div Res, Smithville, TX 78957 USA. RP Morris, MR (reprint author), Ohio Univ, Dept Biol Sci, Athens, OH 45701 USA. NR 41 TC 26 Z9 26 U1 0 U2 2 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD FEB 16 PY 2001 IS 1 BP 65 EP 81 DI 10.1643/0045-8511(2001)001[0065:PRAPON]2.0.CO;2 PG 17 WC Zoology SC Zoology GA 405DP UT WOS:000167142800007 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Wolfgang Laib: A retrospective. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Libs, Washington, DC USA. RP Kalfatovic, MR (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD FEB 15 PY 2001 VL 126 IS 3 BP 164 EP 164 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 401AM UT WOS:000166904800061 ER PT J AU Smith, BD AF Smith, BD TI Documenting plant domestication: The consilience of biological and archaeological approaches SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Editorial Material ID ORIGINS C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20560 USA. RP Smith, BD (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20560 USA. NR 18 TC 79 Z9 83 U1 1 U2 13 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD FEB 13 PY 2001 VL 98 IS 4 BP 1324 EP 1326 DI 10.1073/pnas.98.4.1324 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 401VL UT WOS:000166949200003 PM 11171946 ER PT J AU Piperno, DR Flannery, KV AF Piperno, DR Flannery, KV TI The earliest archaeological maize (Zea mays L.) from highland Mexico: New accelerator mass spectrometry dates and their implications SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID EVOLUTION; TEOSINTE; DOMESTICATION; PHYTOLITHS; LOCUS AB Accelerator mass spectrometry age determinations of maize cobs (Zea mays L,) from Guila Naquitz Cave in Oaxaca, Mexico, produced dates of 5,400 carbon-14 years before the present (about 6,250 calendar years ago), making those cobs the oldest in the Americas. Macrofossils and phytoliths characteristic of wild and domesticated lea fruits are absent from older strata from the site, although Zea pollen has previously been identified from those levels. These results, together with the modern geographical distribution of wild Zea mays, suggest that the cultural practices that led to Zea domestication probably occurred elsewhere in Mexico. Guile Naquitz Cave has now yielded the earliest macrofossil evidence for the domestication of two major American crop plants, squash (Cucurbita pepo) and maize. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Michigan, Museum Anthropol, Ann Arbor, MI 48109 USA. RP Piperno, DR (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama. NR 29 TC 172 Z9 184 U1 3 U2 45 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD FEB 13 PY 2001 VL 98 IS 4 BP 2101 EP 2103 DI 10.1073/pnas.98.4.2101 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 401VL UT WOS:000166949200139 PM 11172082 ER PT J AU Jang-Condell, H Hernquist, L AF Jang-Condell, H Hernquist, L TI First structure formation: A simulation of small-scale structure at high redshift SO ASTROPHYSICAL JOURNAL LA English DT Article DE early universe; galaxies : halos; methods : n-body simulations ID DARK-MATTER HALOES; HIERARCHICAL UNIVERSE; GALAXIES; TREESPH; MODELS; SHAPES AB We describe the results of a simulation of collisionless cold dark matter in a Lambda CDM universe to examine the properties of objects collapsing at high redshift (z = 10). We analyze the halos that form at these early times in this simulation and find that the results are similar to those of simulations of large-scale structure formation at low redshift. In particular, we consider halo properties such as the mass function, density profile, halo shape, spin parameter, and angular momentum alignment with the minor axis. By understanding the properties of small-scale structure formation at high redshift, we can better understand the nature of the first structures in the universe, such as Population III stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jang-Condell, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Jang-Condell, Hannah/0000-0002-7639-1322 NR 31 TC 58 Z9 58 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2001 VL 548 IS 1 BP 68 EP 78 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QN UT WOS:000166939900007 ER PT J AU Matthews, LD Wood, K AF Matthews, LD Wood, K TI Modeling the interstellar medium of low surface brightness galaxies: Constraining internal extinction, disk color gradients, and intrinsic rotation curve shapes SO ASTROPHYSICAL JOURNAL LA English DT Review DE dust, extinction; galaxies : individual (UGC 7321); galaxies : ISM; galaxies : kinematics and dynamics; galaxies : spiral; radiative transfer ID TULLY-FISHER RELATION; EDGE-ON GALAXIES; MONTE-CARLO SIMULATIONS; SMALL-MAGELLANIC-CLOUD; SPIRAL GALAXIES; STAR-FORMATION; DARK-MATTER; MULTIPLE-SCATTERING; RADIATIVE-TRANSFER; CLUMPY MEDIA AB We use a combination of three-dimensional Monte Carlo radiative transfer techniques and multiwavelength (BRHK, H alpha) imaging data to investigate the nature of the interstellar medium (ISM) in the edge-on, low surface brightness (LSB) galaxy UGC 7321. Using realistic models that incorporate multiple scattering effects and clumping of the stars and the interstellar material, we explore the distribution and opacity of the interstellar material (gas+dust) and its effects on the observed stellar disk luminosity profiles, color gradients, and rotation curve shape. We find that UGC 7321 contains a small but nonnegligible dusty component to its ISM, yielding a B-band optical depth <()over bar>(e,B) similar to 4.0 from disk edge to center. A significant fraction (similar to 50% +/- 10%) of the interstellar material in the innermost regions of UGC 7321 appears to be contained in a clumpy medium, indicating that LSB galaxies can support a modest, multiphase ISM structure. In spite of the clear presence of dust, we conclude that the large radial optical color gradients observed in UGC 7321 and other similar LSB spiral galaxies cannot be accounted for by dust and must result primarily from significant stellar population and/or metallicity gradients. We show that realistic optical depth effects will have little impact on the observed rotation curves of edge-on disk galaxies and cannot explain the linear, slowly rising rotation curves seen in some edge-on LSB spirals. Projection effects create a far larger uncertainty in recovering the true underlying rotation curve shape of galaxies viewed at inclinations i greater than or similar to 85 degrees. C1 Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM lmatthew@nrao.edu; kenny@claymore.harvard.edu NR 119 TC 70 Z9 70 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2001 VL 548 IS 1 BP 150 EP 171 DI 10.1086/318687 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QN UT WOS:000166939900013 ER PT J AU Ozel, F Di Matteo, T AF Ozel, F Di Matteo, T TI X-ray images of hot accretion flows SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : nuclei; radiation mechanisms : thermal; X-rays : galaxies ID ADVECTION-DOMINATED ACCRETION; BLACK-HOLE; GALAXY; MODEL; VARIABILITY; TRANSITIONS; TRANSIENTS; QUIESCENCE; DISKS; DISCS AB We consider the X-ray emission due to bremsstrahlung processes from spherically symmetric, low radiative efficiency hot accretion flows around supermassive and galactic black holes. We calculate surface brightness profiles and Michelson visibility functions for a range of density profiles, rho similar to r(-3/2+p), with 0 < p < 1, to allow for the presence of outflows. We find that although the 1 keV emitting region in these flows can always extend up to 10(6) Schwarzschild radii (R-S), their surface brightness profiles and visibility functions are strongly affected by the specific density profile. The advection-dominated solutions with no outflows (p = 0) lead to centrally peaked profiles with characteristic sizes of only a few tens of R-S. Solutions with strong outflows (p similar to 1) lead to flat intensity profiles with significantly larger characteristic sizes of up to 10(6) R-S. This implies that low-luminosity galactic nuclei, such as M87, may appear as extended X-ray sources when observed with current X-ray imaging instruments. We show that X-ray brightness profiles and their associated visibility functions may be powerful probes for determining the relevant mode of accretion and, in turn, the properties of hot accretion flows. We discuss the implications of our results for observations with the Chandra X-Ray Observatory and the proposed X-ray interferometer MAXIM. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ozel, F (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 39 TC 5 Z9 5 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2001 VL 548 IS 1 BP 213 EP 218 DI 10.1086/318658 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QN UT WOS:000166939900017 ER PT J AU Van Dyk, DA Connors, A Kashyap, VL Siemiginowska, A AF Van Dyk, DA Connors, A Kashyap, VL Siemiginowska, A TI Analysis of energy spectra with low photon counts via Bayesian posterior simulation SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods : data analysis; methods : statistical ID X-RAY ASTRONOMY; PARAMETER-ESTIMATION; STATISTICAL-ANALYSIS; DATA AUGMENTATION; MARKOV-CHAINS; DISTRIBUTIONS; EMISSION; STARS; VARIABILITY AB Over the past 10 years Bayesian methods have rapidly grown more popular in many scientific disciplines as several computationally intensive statistical algorithms have become feasible with increased computer power. In this paper we begin with a general description of the Bayesian paradigm for statistical inference and the various state-of-the-art model-fitting techniques that we employ (e.g., the Gibbs sampler and the Metropolis-Hastings algorithm). These algorithms are very flexible and can be used to Dt models that account for the highly hierarchical structure inherent in the collection of high-quality spectra and thus can keep pace with the accelerating progress of new space telescope designs. The methods we develop, which will soon be available in the Chandra Interactive Analysis of Observations (CIAO) software, explicitly model photon arrivals as a Poisson process and thus have no difficulty with high-resolution low-count X-ray and gamma -ray data. We expect these methods to be useful not only for the recently launched Chandra X-Ray Observatory and XMM but also for new generation telescopes such as Constellation X, GLAST, etc. In the context of two examples (quasar S5 0014+813 and hybrid-chromosphere supergiant star alpha TrA), we illustrate a new highly structured model and how Bayesian posterior sampling can be used to compute estimates, error bars, and credible intervals for the various model parameters. Application of our method to the high-energy tail of the ASCA spectrum of alpha TrA confirms that even at a quiescent state, the coronal plasma on this hybrid-chromosphere star is indeed at high temperatures (>10 MK) that normally characterize flaring plasma on the Sun. We are also able to constrain the coronal metallicity and find that although it is subject to large uncertainties, it is consistent with the photospheric measurements. C1 Harvard Univ, Dept Stat, Cambridge, MA 02138 USA. Wellesley Coll, Whitin Observ, Dept Astron, Wellesley, MA 02481 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Van Dyk, DA (reprint author), Harvard Univ, Dept Stat, 1 Oxford St, Cambridge, MA 02138 USA. OI Van Dyk, David/0000-0002-0816-331X NR 54 TC 63 Z9 63 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2001 VL 548 IS 1 BP 224 EP 243 DI 10.1086/318656 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QN UT WOS:000166939900019 ER PT J AU Ojha, R Stark, AA Hsieh, HH Lane, AP Chamberlin, RA Bania, TM Bolatto, AD Jackson, JM Wright, GA AF Ojha, R Stark, AA Hsieh, HH Lane, AP Chamberlin, RA Bania, TM Bolatto, AD Jackson, JM Wright, GA TI AST/RO observations of atomic carbon near the Galactic center SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxy : abundances; galaxy : center; ISM : atoms; ISM : general; ISM : molecules ID INTERSTELLAR-MEDIUM; REGIONS AB We present a coarsely sampled map of the region \l\ less than or equal to 2 degrees, \b\ less than or equal to 0.degrees1 in the 492 GHz (P-3(1) --> P-3(0)) fine-structure transition of neutral carbon, observed with the Antarctic Submillimeter Telescope and Remote Observatory (AST/RO). The distribution of [C I] emission is similar on the large scale to that of CO J = 1 --> 0. On average, the ratio of the integrated intensities, I-[C I]/I-12CO, is higher in the Galactic disk than in the Galactic center region. This result is accounted for by the absorption of (CO)-C-12 within the clouds located in the outer Galactic disk. The ratio I-[C I]/I-12CO is surprisingly uniform over the variety of environments near the Galactic center. On average, [C I] is optically thin [or as optically thin as (CO)-C-13 (J = 1 --> 0)], even in the dense molecular clouds of the Galactic center region. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Caltech Submillimeter Observ, Hilo, HI 96720 USA. Boston Univ, Dept Astron, Boston, MA 02215 USA. Bell Labs, Holmdel, NJ 07733 USA. RP Ojha, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. RI Bania, Thomas/H-2318-2014 NR 20 TC 26 Z9 27 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2001 VL 548 IS 1 BP 253 EP 257 DI 10.1086/318693 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QN UT WOS:000166939900022 ER PT J AU Rakowski, CE Hughes, JP Slane, P AF Rakowski, CE Hughes, JP Slane, P TI Two new ejecta-dominated Galactic supernova remnants: G337.2-0.7 and G309.2-0.6 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; supernova remnants; X-rays : general ID EMISSION; CASSIOPEIA; ABUNDANCES; CATALOG AB We present the analysis of new X-ray observations of two Galactic radio supernova remnants (SNRs), G337.2-0.7 and G309.2-0.6. Both remnants exhibit line-rich thermal spectra that require highly nonsolar elemental abundance ratios. In each case, Si and S are unequivocally overabundant compared to solar, based purely on the measured equivalent width of the K alpha line complex. Detailed nonequilibrium ionization spectral analysis of these remnants, using a single-temperature, single ionization age model, confirms the overabundances, yielding Si, S, and Ar abundances many times their solar values : 3-5 times solar for G337.2-0.7 and greater than 3-10 times solar for G309.2-0.6. We also find that for both remnants, Ne and Mg are underabundant relative to Si, and for G309.2-0.6, Ca and Fe are relatively underabundant as well. This is the first detection of metal-rich, nonsolar abundance material in these remnants, identifying them as young ejecta-dominated SNRs. Further support for their youth comes from the distances that we estimate from the fitted column densities (less than 15 kpc for G337.2-0.7, and 4 +/- 2 kpc for G309.2-0.6). From the implied sizes of the remnants at these distances we infer relatively young ages (2000-4500 years for G337.2-0.7 and 700-4000 years for G309.2-0.6). Finally, we note that no compact object has yet been found within G337.2-0.7, but an X-ray point source is evident within the radio shell of G309.2-0.6, although its nature remains unknown. C1 Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. CEA Saclay, Serv Astrophys, Orme Merisiers, F-91191 Gif Sur Yvette, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rakowski, CE (reprint author), Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. NR 28 TC 11 Z9 11 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2001 VL 548 IS 1 BP 258 EP 268 DI 10.1086/318680 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QN UT WOS:000166939900023 ER PT J AU Kamazaki, T Saito, M Hirano, N Kawabe, R AF Kamazaki, T Saito, M Hirano, N Kawabe, R TI Millimeter-wave interferometric study of the p Ophiuchi A region. I. Small-scale structures of dust continuum sources SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : individual (p Ophiuchi); stars : formation; ISM : jets and outflows; ISM : molecules; radio lines : ISM ID YOUNG STELLAR OBJECTS; MAGNETIC-FIELD STRUCTURE; SHEET-LIKE CLOUDS; STAR-FORMATION; DENSE CORES; INITIAL CONDITIONS; DARK CLOUDS; VLA 1623; FRAGMENTATION; PROTOSTARS AB We performed 3 mm continuum and (CO)-C-12 (J = 1-0) line observations of the rho Ophiuchi A region using the Nobeyama Millimeter Array. The high-resolution dust continuum map reveals that the two submillimeter sources (SM1 and SM1N), which are considered to be pre-protostellar cores, consist of smaller scale fragments of 600-1100 AU in size. The small fragments lie along two filamentary features that cross each other at the position close to SM1, with a typical projected separation of 1200 AU. This is the first detection of such small-scale fragments in pre-protostellar cores from dust continuum observations. The masses and densities of the small fragments are estimated to be 0.054-0.14 M. and (2.0- 15) x 10(7) cm(-3), respectively, and they appear to be gravitationally bound. From our CO observations, we have discovered a previously unknown CO outflow whose axis is almost parallel to that of the nearby outflow associated with VLA 1623. However, the center of this outflow is likely to be the near-infrared source GY 30, and does not coincide with any of the small fragments. All small fragments except one show no sign of protostellar activities such as CO outflow and centimeter radio continuum emission, suggesting that they are in the evolutionary stage prior to protostar formation with outflow activities. On the other hand, the small fragment with the largest mass is likely to be associated with 6 cm continuum emission, which is thought to be free-free emission. This implies the possibility that the protostellar formation has already occurred in the fragment. The presence of small-scale fragments with and without protostellar activities suggests that star formation in this region occur in such a small fragment or through coalescence of several small fragments. C1 Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Grad Univ Adv Studies, Natl Astron Observ, Dept Astron Sci, Tokyo 1818588, Japan. Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. RP Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. EM kamazaki@nro.nao.ac.jp NR 35 TC 15 Z9 15 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2001 VL 548 IS 1 BP 278 EP 287 DI 10.1086/318668 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QN UT WOS:000166939900025 ER PT J AU Jayawardhana, R Hartmann, L Calvet, N AF Jayawardhana, R Hartmann, L Calvet, N TI Infall models of class 0 protostars SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; radiative transfer; stars : formation; stars : pre-main-sequence ID YOUNG STELLAR OBJECTS; AURIGA MOLECULAR CLOUD; T-TAURI STARS; OPHIUCHI CLOUD; INITIAL CONDITIONS; PROTOSTELLAR COLLAPSE; DENSE CORES; SUBMILLIMETER; DISCOVERY; ACCRETION AB We have carried out radiative transfer calculations of infalling, dusty envelopes surrounding embedded protostars to understand the observed properties of the recently identified "class 0" sources. To match the far-infrared peaks in the spectral energy distributions of objects such as the prototype class 0 source VLA 1623, pure collapse models require mass infall rates similar to 10(-4) yr(-1). The radial intensity distributions predicted by such infall models are inconsistent with observations of VLA 1623 at submillimeter wavelengths, in agreement with the 1993 results of and coworkers who found a density profile of Andre and rho proportional to r(-1/2) rather than the expected rho proportional to r(-3/2) gradient. To resolve this conflict while still invoking infall to produce the outflow source at the center of VLA 1623, we suggest that the observed submillimeter intensity distribution is the sum of two components: an inner infall zone plus an outer, more nearly constant density region. This explanation of the observations requires that roughly half the total mass observed within a 2000 AU radius of the source lies in a region external to the infall zone. The column densities for this external region are comparable to those found in the larger Oph A cloud within which VLA 1623 is embedded. This decomposition into infall and external regions is not unique, owing to uncertainty in the structure of the molecular gas outside of the infall zone, which in turn implies some uncertainty in estimating the infall rate. Nevertheless, the environment of Oph A is so dense that any protostellar clouds that fragment out are likely to collapse at very high infall rates, consistent with our spectral energy distribution modeling. The extreme environments of class 0 sources lead us to suggest an alternative or additional interpretation of these objects: rather than simply concluding with and Andre and coworkers that class 0 objects represent only the earliest phases of protostellar collapse and ultimately evolve into older "class I" protostars, we suggest that many class 0 sources could be the protostars of very dense regions, and class I objects found in lower density regions may be in comparable evolutionary states. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jayawardhana, R (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. NR 58 TC 26 Z9 26 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2001 VL 548 IS 1 BP 310 EP 317 DI 10.1086/318650 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QN UT WOS:000166939900028 ER PT J AU Tomsick, JA Kaaret, P AF Tomsick, JA Kaaret, P TI The X-ray properties of low-frequency quasi-periodic oscillations from GRS 1915+105 up to 120 keV SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; black hole physics; stars : individual (GRS 1915+105); X-rays : stars ID RXTE OBSERVATIONS; GRS-1915+105; STATES AB We present a study of the properties of strong 0.8-3.0 Hz quasi-periodic oscillations (QPOs) that occurred during 1997 Rossi X-Ray Timing Explorer (RXTE) observations of the microquasar GRS 1915 + 105 in the low-hard state. The high count rates allow us to track individual QPO peaks, and we exploit this to develop a QPO folding technique. In contrast to previous QPO studies with RXTE, we emphasize the high-energy QPO properties and report the detection of a QPO in the 60-124 keV energy band. Our technique allows us, for the first time, to measure the phase of the QPO harmonics relative to the fundamental. Variation in this phase difference leads to changes in the shape of the QPO profile with energy and over time. The strength of the QPO fundamental increases up to 19 keV, but the data do not suggest that the strength continues to increase above this energy. In some cases, the QPO amplitudes in the 30-60 and 60-124 keV energy bands are significantly less than in the 13-19 and 19-29 keV energy bands. We also use our technique to measure the phase lag of the QPO fundamental and harmonics. In the case where negative phase lags are detected for the fundamental, positive phase lags are detected for the second harmonic. C1 Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tomsick, JA (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr,Code 0424, La Jolla, CA 92093 USA. NR 17 TC 34 Z9 35 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2001 VL 548 IS 1 BP 401 EP 409 DI 10.1086/318683 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QN UT WOS:000166939900036 ER PT J AU Drake, JJ Brickhouse, NS Kashyap, V Laming, JM Huenemoerder, DP Smith, R Wargelin, BJ AF Drake, JJ Brickhouse, NS Kashyap, V Laming, JM Huenemoerder, DP Smith, R Wargelin, BJ TI Enhanced noble gases in the coronae of active stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : abundances; stars : activity; stars : coronae; stars : late-type; Sun : corona; X-rays : stars ID ASCA OBSERVATIONS; RAY MEASUREMENTS; AR LACERTAE; SOLAR; ABUNDANCES; EMISSION; HELIUM; EUVE; TEMPERATURE; ELEMENTS AB We have analyzed Chandra High-Energy Transmission Grating spectra of the active RS CVn-type binary V711 Tauri (HR 1099; HD 22468) in order to examine the chemical composition of its coronae. Observed fluxes and flux upper limits for spectral lines from a range of charge states of iron, covering species Fe XVI- Fe XXV, have been used to determine the emission measure distribution as a function of temperature, while the observed Fe line-to-continuum ratio has been used to examine the absolute iron abundance, Fe/H. Abundances of elements O, Ne, Mg, Si, S, and Ar relative to both Fe and H have been estimated by comparison of observed line fluxes with predictions based on the emission measure distribution. We confirm results of earlier studies finding the coronae of V711 Tau to be metal-poor and derive an iron abundance of Fe/H = 7.0 +/- 0.1. We find the noble gas elements Ne and Ar to be enhanced relative to the local cosmic value and enhanced by an order of magnitude relative to Fe. Very mild enhancements of O and Mg relative to Fe are also discerned. By examination of coronal abundances of Ne relative to Fe culled from the literature, in addition to Ne lines seen in hitherto unpublished Chandra spectra, we conclude that large Ne abundance enhancements are a common feature of active stellar coronae. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. USN, EO Hulburt Ctr Space Res, Res Lab, Washington, DC 20375 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Drake, JJ (reprint author), Harvard Smithsonian Ctr Astrophys, MS-3,60 Garden St, Cambridge, MA 02138 USA. OI Brickhouse, Nancy/0000-0002-8704-4473 NR 34 TC 76 Z9 76 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2001 VL 548 IS 1 BP L81 EP L85 DI 10.1086/318933 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QV UT WOS:000166940500020 ER PT J AU Woodard, MF Korzennik, SG Rabello-Soares, MC Kumar, P Tarbell, TD Acton, S AF Woodard, MF Korzennik, SG Rabello-Soares, MC Kumar, P Tarbell, TD Acton, S TI Energy distribution of solar oscillation modes inferred from space-based measurements SO ASTROPHYSICAL JOURNAL LA English DT Article DE convection; Sun : oscillations; turbulence AB We have measured the energy distribution of solar p- and f-mode oscillations of angular degree and temporal frequency in the range 100 < l < 800 and 2 < v(mHz) < 4 using helioseismology data from the Solar Oscillations Investigation-Michelson Doppler Imager instrument on the Solar and Heliospheric Observatory satellite. At temporal frequency v approximate to 3 mHz, the surface velocity power per oscillation mode increases slightly with angular degree between l = 100 and l = 2000 but decreases rather steeply with l above l = 200, in approximate agreement with earlier findings from ground-based measurements. From this we infer that the time-averaged energy per mode, which is theoretically related to the modal surface velocity power, decreases steeply with, at fixed l frequency, over the entire observed l-range. Specifically, at v = 3.1 mHz, the energy per mode drops by a factor of approximate to 10 between l = 150 and l = 650, a circumstance not quantitatively understood at present. C1 New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Stanford Univ, HEPL, Stanford, CA 94305 USA. Inst Adv Study, Princeton, NJ 08540 USA. Lockheed Martin, Palo Alto Res Lab, Palo Alto, CA 94304 USA. WM Keck Observ, Kamuela, HI 96743 USA. RP Woodard, MF (reprint author), New Jersey Inst Technol, Big Bear Solar Observ, 40386 N Shore Lane, Big Bear City, CA 92314 USA. RI Rabello Soares, Maria Cristina/C-3207-2013; OI Rabello Soares, Maria Cristina/0000-0003-0172-3713 NR 14 TC 8 Z9 8 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2001 VL 548 IS 1 BP L103 EP L106 DI 10.1086/318935 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QV UT WOS:000166940500025 ER PT J AU Kress, WJ Miller, SE Krupnick, GA Lovejoy, TE AF Kress, WJ Miller, SE Krupnick, GA Lovejoy, TE TI Museum collections and conservation efforts SO SCIENCE LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. Smithsonian Inst, Natl Museum Nat Hist, Plant Conservat Unit, Washington, DC 20560 USA. Smithsonian Inst, Natl Museum Nat Hist, Off Secretary Sci, Washington, DC 20560 USA. RP Kress, WJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. NR 3 TC 9 Z9 9 U1 4 U2 10 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD FEB 2 PY 2001 VL 291 IS 5505 BP 828 EP 829 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 398TD UT WOS:000166771700025 PM 11225629 ER PT J AU Silva, S AF Silva, S TI Questioning misfortune: The pragmatics of uncertainty in eastern Uganda. SO AMERICAN ETHNOLOGIST LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Silva, S (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 2 U2 2 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 USA SN 0094-0496 J9 AM ETHNOL JI Am. Ethnol. PD FEB PY 2001 VL 28 IS 1 BP 216 EP 217 DI 10.1525/ae.2001.28.1.216 PG 2 WC Anthropology SC Anthropology GA 483LX UT WOS:000171628400016 ER PT J AU Jantz, RL Owsley, DW AF Jantz, RL Owsley, DW TI Variation among early North American crania SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE Paleoamericans; cranial morphometrics; New World ID MTDNA HAPLOGROUP-X; HUMAN REMAINS; NEW-WORLD; POPULATIONS; ORIGINS; PALEOINDIANS; AMERINDIANS AB The limited morphometric work on early American crania to date has treated them as a single, temporally defined group. This paper addresses the question of whether there is significant variability among ancient American crania. A sample of 11 crania (Spirit Cave, Wizards Beach, frowns Valley, Pelican Rapids, Prospect, Wet Gravel male, Wet Gravel female, Medicine Crow, Turin, Lime Creek, and Swanson Lake) dating from the early to mid Holocene was available. Some have recent accelerator mass spectrometry AMS dates, while others are dated geologically or archaeologically. All are in excess of 4500 BP, and most are 7000 BP or older. Measurements follow the definitions of Howells [(1973) Cranial variation in man, Cambridge: Harvard University). Some crania are incomplete, but 22 measurements were common to all fossils. Cranial variation was examined by calculating the Mahalanobis distance between each pair of fossils, using a pooled within sample covariance matrix estimated from the data of Howells. The distance relationships among crania suggest the presence of at least three distinct groups: I) a middle Archaic Plains group (Turin and Medicine Crow), 2) a Paleo/Early Archaic Great Lakes/Plains group (Browns Valley, Pelican Rapids, Lime Creek), and 3) a spatially and temporally heterogeneous group that includes the Great Basin/Pacific Coast (Spirit Cave, Wizards Beach, Prospect) and Nebraska (Wet Gravel specimens and Swanson Lake). These crania were also compared to Howells' worldwide recent sample, which was expanded by including six additional American Indian samples. None of the fossils, except for the Wet Gravel male, shows any particular affinity to recent Native Americans; their greatest similarities are with Europe, Polynesia, or East Asia. Several crania would be atypical in any recent population for which we have data. Browns Valley, Pelican Rapids, and Lime Creek are the most distinctive. They provide evidence for the presence of an early population that bears no similarity to the morphometric pattern of recent American Indians or even to crania of comparable date in other regions of the continent. The heterogeneity among early American crania makes it inadvisable to pool them for purposes of morphometric analysis. Whether this heterogeneity results from different early migrations or one highly differentiated population cannot be established from our data. Our results are inconsistent with hypotheses of an ancestor-descendent relationship between early and late Holocene American populations. They suggest that the pattern of cranial variation is of recent origin, at least in the Plains region. (C) 2001 Wiley-Liss, Inc. C1 Univ Tennessee, Dept Anthropol, Knoxville, TN 37996 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP Jantz, RL (reprint author), Univ Tennessee, Dept Anthropol, Knoxville, TN 37996 USA. NR 63 TC 75 Z9 78 U1 0 U2 10 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD FEB PY 2001 VL 114 IS 2 BP 146 EP 155 DI 10.1002/1096-8644(200102)114:2<146::AID-AJPA1014>3.0.CO;2-E PG 10 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 398PA UT WOS:000166763800005 PM 11169904 ER PT J AU Carbone, C Christie, S Conforti, K Coulson, T Franklin, N Ginsberg, JR Griffiths, M Holden, J Kawanishi, K Kinnaird, M Laidlaw, R Lynam, A Macdonald, DW Martyr, D McDougal, C Nath, L O'Brien, T Seidensticker, J Smith, DJL Sunquist, M Tilson, R Shahruddin, WNW AF Carbone, C Christie, S Conforti, K Coulson, T Franklin, N Ginsberg, JR Griffiths, M Holden, J Kawanishi, K Kinnaird, M Laidlaw, R Lynam, A Macdonald, DW Martyr, D McDougal, C Nath, L O'Brien, T Seidensticker, J Smith, DJL Sunquist, M Tilson, R Shahruddin, WNW TI The use of photographic rates to estimate densities of tigers and other cryptic mammals SO ANIMAL CONSERVATION LA English DT Article AB The monitoring and management of species depends on reliable population estimates, and this can be both difficult and very costly for cryptic large vertebrates that live in forested habitats. Recently developed camera trapping techniques have already been shown to be an effective means of making mark-recapture estimates of individually identifiable animals (e.g. tigers). Camera traps also provide a new method for surveying animal abundance. Through computer simulations, and an analysis of the rates of camera trap capture from 19 studies of tigers across the species' range, we show that the number of camera days/tiger photograph correlates with independent estimates of tiger density. This statistic does not rely on individual identity and is particularly useful for estimating the population density of species that are not individually identifiable. Finally, we used the comparison between observed trapping rates and the computer simulations to estimate the minimum effort required to determine that tigers. or other species, do not exist in an area, a measure that is critical for conservation planning. C1 Zool Soc London, Inst Zool, London NW1 4RY, England. Zool Soc London, London Zoo, London NW1 4RY, England. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Univ York, Dept Biol, York YO1 5DD, N Yorkshire, England. Sumatran Tiger Project, Lampung 34101, Sumatra, Indonesia. Wildlife Conservat Soc, Int Programs, Bronx, NY 10460 USA. Leuser Dev Program, Medan 20154, Sumatra, Indonesia. Fauna & Flora Int, Cambridge CB1 2DT, England. Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. Univ Oxford, Dept Zool, Wildlife Conservat Res Unit, Oxford OX1 3PS, England. Tiger Tops, Kathmandu, Nepal. Univ Minnesota, Dept Fisheries & Wildlife, St Paul, MN 55108 USA. RP Carbone, C (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England. OI Lynam, Antony/0000-0002-8395-7902; Coulson, Tim/0000-0001-9371-9003 NR 13 TC 203 Z9 231 U1 9 U2 111 PU CAMBRIDGE UNIV PRESS PI PORT CHESTER PA 110 MIDLAND AVE, PORT CHESTER, NY 10573-4930 USA SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD FEB PY 2001 VL 4 BP 75 EP 79 DI 10.1017/S1367943001001081 PN 1 PG 5 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 428QA UT WOS:000168471300008 ER PT J AU Sayre, EV Joel, EC Blackman, MJ Yener, KA Ozbal, H AF Sayre, EV Joel, EC Blackman, MJ Yener, KA Ozbal, H TI Stable lead isotope studies of Black Sea Anatolian ore sources and related Bronze Age and Phrygian artefacts from nearby archaeological sites. Appendix: New Central Taurus ore data SO ARCHAEOMETRY LA English DT Article DE Black Sea; central Taurus; Anatolia; metal; ores; artefacts; Bronze Age; multivariate; statistics; probabilities ID MULTIVARIATE NORMALITY AB The accumulated published database of stable lead isotope analyses of ore and slag specimens taken from Anatolian mining sites that parallel the Black Sea coast has been augmented with 22 additional analyses of such specimens carried out at the National Institute of Standards and Technology. Multivariate statistical analysis has been used to divide this composite database into five separate ore source groups. Evidence that most of these ore sources were exploited for the production of metal artefacts during the Bronze Age and Phrygian Period has been obtained by statistically comparing to tem the isotope ratios of 184 analysed artefacts from nine archaeological sites situated within a few hundred kilometres of these mining sites. Also, Appendix B contains 36 new isotope analyses of ore specimens from Central Taurus mining sites that are compatible with and augment the four Central Taurus Ore Source Groups defined in Yener et al. (1991). C1 Smithsonian Inst, Smithsonian Ctr Materials Res & Educ, Washington, DC 20560 USA. Univ Chicago, Oriental Inst, Chicago, IL 60637 USA. Bogazici Univ, Fac Arts & Sci, Istanbul, Turkey. RP Sayre, EV (reprint author), Smithsonian Inst, Smithsonian Ctr Materials Res & Educ, Washington, DC 20560 USA. NR 44 TC 18 Z9 18 U1 0 U2 6 PU OXFORD UNIV PI OXFORD PA RES LAB ARCHAEOL HIST ART 6 KEBLE RD, OXFORD OX1 3QJ, ENGLAND SN 0003-813X J9 ARCHAEOMETRY JI Archaeometry PD FEB PY 2001 VL 43 BP 77 EP 115 DI 10.1111/1475-4754.00006 PN 1 PG 39 WC Archaeology; Chemistry, Analytical; Chemistry, Inorganic & Nuclear; Geosciences, Multidisciplinary SC Archaeology; Chemistry; Geology GA 409RN UT WOS:000167398100006 ER PT J AU Barton, EJ Geller, MJ Bromley, BC van Zee, L Kenyon, SJ AF Barton, EJ Geller, MJ Bromley, BC van Zee, L Kenyon, SJ TI The Tully-Fisher relation as a measure of luminosity evolution: A low-redshift baseline for evolving galaxies SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : fundamental parameters; galaxies : interactions; galaxies : kinematics and dynamics; galaxies : spiral ID EMISSION-LINE GALAXIES; HUBBLE DEEP FIELD; EXTRAGALACTIC DISTANCE SCALE; PHOTOMETRIC STANDARD STARS; PECULIAR VELOCITY ANALYSIS; OPTICAL-ROTATION CURVES; LOCAL CONVERGENCE DEPTH; SPIRAL GALAXIES; COMPACT GALAXIES; SC GALAXIES AB We use optical rotation curves to investigate the R-band Tully-Fisher properties of a sample of 90 spiral galaxies in close pairs, covering a range of luminosities, morphological types, and degrees of tidal distortion. The galaxies follow the Tully-Fisher relation remarkably well, with the exception of eight distinct similar to3 sigma outliers. Although most of the outliers show signs of recent star formation, gasdynamical effects are probably the dominant cause of their anomalous Tully-Fisher properties. Four outliers with small emission-line widths have very centrally concentrated line emission and truncated rotation curves; the central emission indicates recent gas infall after a close galaxy-galaxy pass. These four galaxies may be local counterparts to compact, blue galaxies at intermediate redshift. The remaining galaxies have a negligible offset from the reference Tully-Fisher relation, but a shallower slope (2.6 sigma significance) and a 25% larger scatter. We argue that triggered star formation is a significant contributor to the slope difference. We characterize the nonoutlier sample with measures of distortion and star formation to search for third-parameter dependence in the residuals of the TF relation. Severe kinematic distortion is the only significant predictor of TF residuals; this distortion is not, however, responsible for the slope difference from the reference distribution. Because the outliers are easily removed by sigma clipping, we conclude that even in the presence of some tidal distortion, detection of moderate (greater than or similar to0.5 mag in rest-frame R) luminosity evolution should be possible with high-redshift samples the size of this 90-galaxy study. The slope of the TF relation, although difficult to measure, is as fundamental for quantifying luminosity evolution as the zero-point offset. C1 Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Barton, EJ (reprint author), Natl Res Council Canada, Herzberg Inst Astrophys, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. OI Kenyon, Scott/0000-0003-0214-609X NR 71 TC 40 Z9 40 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2001 VL 121 IS 2 BP 625 EP 648 DI 10.1086/318759 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QL UT WOS:000166939700005 ER PT J AU Rose, JA Gaba, AE Caldwell, N Chaboyer, B AF Rose, JA Gaba, AE Caldwell, N Chaboyer, B TI Starbursts versus truncated star formation in nearby clusters of galaxies SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : elliptical and lenticular, cD; galaxies : evolution; galaxies : interactions; galaxies : starburst; intergalactic medium ID DISTANT CLUSTERS; COMA CLUSTER; DISK GALAXIES; VIRGO CLUSTER; SURFACE PHOTOMETRY; MERGING GALAXIES; COLOR GRADIENTS; RICH CLUSTERS; EVOLUTION; MERGER AB We present long-slit spectroscopy, B- and R-bandpass imaging, and 21 cm observations of a sample of early-type galaxies in nearby clusters, which are known to be either in a star-forming phase or to have had star formation that recently terminated. From the long-slit spectra, obtained with the Blanco 4 m telescope, we find that emission lines in the star-forming cluster galaxies are significantly more centrally concentrated than in a sample of field galaxies. The broadband imaging reveals that two currently star-forming early-type galaxies in the Pegasus I cluster have blue nuclei, again indicating that recent star formation has been concentrated. In contrast, the two galaxies for which star formation has already ended show no central color gradient. The Pegasus I galaxy with the most evident signs of ongoing star formation (NGC 7648), exhibits signatures of a tidal encounter. Neutral hydrogen observations of that galaxy with the Arecibo radio telescope reveal the presence of similar to4 x 10(8) M. of H I. Arecibo observations of other current or recent star-forming early-type galaxies in Pegasus I indicate smaller amounts of gas in one of them, and only upper limits in others. These observations indicate that NGC 7648 in the Pegasus I cluster owes its present star formation episode to some form of tidal interaction. The same may be true for the other galaxies with centralized star formation, but we cannot rule out the possibility that their outer disks have been removed via ram pressure stripping, followed by rapid quenching of star formation in the central region. C1 Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. Smithsonian Inst, FL Whipple Observ, Amado, AZ 85645 USA. Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. RP Rose, JA (reprint author), Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. OI Chaboyer, Brian/0000-0003-3096-4161 NR 59 TC 31 Z9 31 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2001 VL 121 IS 2 BP 793 EP 807 DI 10.1086/318754 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QL UT WOS:000166939700016 ER PT J AU Macri, LM Stanek, KZ Sasselov, DD Krockenberger, M Kaluzny, J AF Macri, LM Stanek, KZ Sasselov, DD Krockenberger, M Kaluzny, J TI The direct project: Catalogs of stellar objects in nearby galaxies. I. The central part of M33 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : individual (M33); galaxies : stellar content ID DETACHED ECLIPSING BINARIES; DIRECT DISTANCES; VARIABLES; PHOTOMETRY; CEPHEIDS AB The DIRECT project aims to determine direct distances to two important galaxies in the cosmological distance ladder-M31 and M33-using detached eclipsing binaries (DEBs) and Cepheids. The search for these variables requires time-series photometry of large areas of the target galaxies and yields magnitudes and positions for tens of thousands of stellar objects, which may be of use to the astronomical community at large. During the first phase of the project, between 1996 September and 1997 October, we were awarded 95 nights on the F. L. Whipple Observatory 1.2 m telescope and 36 nights on the Michigan-Dartmouth-MIT 1.3 m telescope to search for DEBs and Cepheids in the M31 and M33 galaxies. This paper, the first in our series of stellar catalogs, lists the positions, three-color photometry, and variability indices of 57,581 stars with 14.4 < V < 23.6 in the central part of M33. The catalog is available from our FTP site. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. N Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Macri, LM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 18 TC 22 Z9 22 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2001 VL 121 IS 2 BP 861 EP 869 DI 10.1086/318772 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QL UT WOS:000166939700020 ER PT J AU Macri, LM Stanek, KZ Sasselov, DD Krockenberger, M Kaluzny, J AF Macri, LM Stanek, KZ Sasselov, DD Krockenberger, M Kaluzny, J TI Direct distances to nearby galaxies using detached eclipsing binaries and Cepheids. VI. Variables in the central part of M331 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; Cepheids; distance scale; galaxies : individual (M33); stars : variables : other ID FIELD; STARS AB The DIRECT project aims to determine direct distances to two important galaxies in the cosmological distance ladder-M31 and M33-using detached eclipsing binaries (DEBs) and Cepheids. We present the results of the first large-scale CCD-based search for variables in M33. We have observed two fields located in the central region of M33 for a total of 95 nights on the F. L. Whipple Observatory 1.2 m telescope and 36 nights on the Michigan-Dartmouth-MIT 1.3 m telescope. We have found a total of 544 variables, including 251 Cepheids and 47 eclipsing binaries. The catalog of variables is available on-line, long with finding charts and BVI light curve data (consisting of 8.2 x 10(4) individual measurements). The complete set of CCD frames is available upon request. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. N Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Macri, LM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 21 TC 34 Z9 34 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2001 VL 121 IS 2 BP 870 EP 890 DI 10.1086/318773 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QL UT WOS:000166939700021 ER PT J AU Gomez, M Kenyon, SJ AF Gomez, M Kenyon, SJ TI A near-infrared imaging survey of the chamaeleon I dark cloud SO ASTRONOMICAL JOURNAL LA English DT Article DE dust, extinction; ISM : individual (Chamaeleon I); stars : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID MOLECULAR CLOUD; T-ASSOCIATION; ISOCAM OBSERVATIONS; SPACE DISTRIBUTION; STAR COUNTS; EXTINCTION; GALAXIES; POPULATION; PHOTOMETRY; SYSTEMS AB We describe a near-infrared imaging survey covering similar to 1 deg(2) of the Chamaeleon I dark cloud. The survey is complete for K < 15.0, H < 16.0, and J < 16.5, roughly 2 magnitudes more sensitive than previous large-scale surveys. We use the large number of background stars detected to derive an accurate near-infrared extinction law for the cloud and select new candidate members with near-infrared color excesses. We list 100 candidates of the cloud with K greater than or equal to 12.0, based on their positions in the J-H, H-K color-color diagram. These new stars have low luminosities (K similar to 12-16, and H-K greater than or similar to 0.5-1.5) may have masses close to or even below the hydrogen-burning limit. C1 Observ Astron, RA-5000 Cordoba, Argentina. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Gomez, M (reprint author), Observ Astron, Laprida 854, RA-5000 Cordoba, Argentina. EM mercedes@oac.uncor.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X NR 49 TC 41 Z9 41 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2001 VL 121 IS 2 BP 974 EP 983 DI 10.1086/318776 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QL UT WOS:000166939700027 ER PT J AU Hartmann, L AF Hartmann, L TI On age spreads in star-forming regions SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; stars : formation; stars : pre-main-sequence ID T-TAURI STARS; MAIN-SEQUENCE STARS; ORION NEBULA CLUSTER; X-RAY; STELLAR BIRTHLINE; MOLECULAR CLOUD; MAGNETIC-FIELD; DISK ACCRETION; AURIGA; EMISSION AB I consider current observational constraints on age spreads in star-forming regions and recent attempts to infer the star-forming histories of molecular cloud complexes. My analysis concentrates on low-mass pre-main-sequence stars on Hayashi tracks, which constitute the bulk of the stellar population. Current observational and theoretical uncertainties probably preclude any robust inferences of the detailed variation of star formation rates as a function of time. These results do not change the conclusion, supported again recently by the systematic study of Palla & Stahler, that star formation is rapid. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hartmann, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 48 TC 152 Z9 152 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2001 VL 121 IS 2 BP 1030 EP 1039 DI 10.1086/318770 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QL UT WOS:000166939700033 ER PT J AU McGary, RS Brisken, WF Fruchter, AS Goss, WM Thorsett, SE AF McGary, RS Brisken, WF Fruchter, AS Goss, WM Thorsett, SE TI Proper-motion measurements with the VLA. I. Wide-field imaging and pulse-gating techniques SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; pulsars : general; techniques : interferometric AB The pulsar velocity distribution provides information about the binary history of pulsar progenitors, as well as the asymmetries of the supernova events in which pulsars are born. Studies of local pulsars present a biased view of this distribution, because they preferentially select low-velocity pulsars that have remained near their birthplaces in the Galactic plane. Using the VLA, we have studied the proper motions of a large sample of distant pulsars. These pulsars are generally faint, and the expected proper motions are small. In this paper, we describe the data analysis techniques that we have developed to allow precise astrometric measurements of faint sources with the VLA. These techniques include "gating" the VLA correlator to increase the signal-to-noise ratio of the pulsar by gathering data only during the pulse. Wide-field imaging techniques, including multiband imaging to account for bandwidth smearing, were used to allow identification of multiple in-beam background sources for astrometric calibration. We present the analysis of three pulsars and demonstrate that astrometric accuracy of about 10 mas can be obtained for individual sources with our technique, allowing measurement of proper motions with errors of only a few milliarcseconds per year over our 7 year baseline. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP McGary, RS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 10, Cambridge, MA 02138 USA. NR 8 TC 11 Z9 11 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2001 VL 121 IS 2 BP 1192 EP 1198 DI 10.1086/318739 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 401QL UT WOS:000166939700049 ER PT J AU White, M AF White, M TI The mass of a halo SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods : N-body simulations ID COLD DARK-MATTER; UNIVERSE AB We discuss the different definitions of the mass of a halo in common use and how one may convert between them. Using N-body simulations we show that mass estimates based on spherical averages are much more tightly correlated with each other than with masses based on the number of particles in a halo. The mass functions pertaining to some different mass definitions are estimated and compared to the "universal form" of Jenkins ct al. (2000). Using a different simulation pipeline and a different cosmological model we show that the mass function is well fit by the Jenkins et al. (2000) fitting function, strengthening the claim to universality made by those authors. We show that care must be taken to match the definitions of mass when using large N-body simulations to bootstrap scaling relations from smaller hydrodynamical runs to avoid observationally significant bias in the predictions for abundances of objects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP White, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mwhite@cfa.harvard.edu RI White, Martin/I-3880-2015 OI White, Martin/0000-0001-9912-5070 NR 15 TC 108 Z9 108 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2001 VL 367 IS 1 BP 27 EP 32 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 410KW UT WOS:000167440000003 ER PT J AU Guenther, EW Torres, G Batalha, N Joergens, V Neuhauser, R Vijapurkar, J Mundt, R AF Guenther, EW Torres, G Batalha, N Joergens, V Neuhauser, R Vijapurkar, J Mundt, R TI RX J1603.8-3938 - a surprising pre-main sequence spectroscopic binary SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : binaries : spectroscopic; stars : formation; stars : late-type; stars : pre-main sequence ID SOLAR-TYPE STARS; T-TAURI STARS; FORMING REGION; LUPUS; EVOLUTION AB We have determined the orbit of the double-lined spectroscopic binary RX J1603.8-3938. The binary consists of two weak-line T Tauri stars, both of which have a spectral type between K3 and K4. The period of the circular orbit is 7.55626 +/- 0.00021 days and the mass ratio 0.9266 +/- 0.0963. To our knowledge RX J1603.8-3938 is thus the pre-main sequence binary with the longest period that has a circular orbit. Despite the fact that the masses and spectral types of the two components are almost identical, the photospheric lines are much stronger in one component than in the other. In the wavelength region between 5500 and 7800 Angstrom we find that the ratio of the equivalent widths of the primary to the secondary is 0.60 +/- 0.03. This ratio is constant in time: and is the same for all photospheric lines. Since the components are weak-line T Tauri stars, the effect cannot be explained by any kind of veiling. We are led to the conclusion that the secondary is 0.55 +/- 0.05 mag fainter than the primary. It thus turns out that evolutionary tracks of pre-main sequence single stars are unable to explain the position of this system in the HR diagram. C1 Karl Schwarzschild Observatorium, Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Nacl Rio De Janeiro, Dept Astrofis, BR-20921 Rio De Janeiro, RJ, Brazil. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Homi Bhabha Ctr Sci Educ, Tata Inst Fundamental Res, Bombay 400088, Maharashtra, India. Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Guenther, EW (reprint author), Karl Schwarzschild Observatorium, Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany. NR 21 TC 10 Z9 10 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2001 VL 366 IS 3 BP 965 EP 971 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 404ZA UT WOS:000167131600026 ER PT J AU Green, DWE Marsden, DG Morris, CS AF Green, DWE Marsden, DG Morris, CS TI Brightness predictions for comets SO ASTRONOMY & GEOPHYSICS LA English DT Editorial Material C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Green, DWE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 22 TC 1 Z9 1 U1 0 U2 1 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 1366-8781 J9 ASTRON GEOPHYS JI Astron. Geophys. PD FEB PY 2001 VL 42 IS 1 BP 11 EP 12 DI 10.1046/j.1468-4004.2001.0420011.11.x PG 2 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA 404ZF UT WOS:000167132200011 ER PT J AU Metzler, CA White, M Loken, C AF Metzler, CA White, M Loken, C TI The effect of the cosmic web on cluster weak lensing mass estimates SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; galaxies : clusters : general; gravitational lensing ID X-RAY-EMISSION; GALAXY CLUSTERS; DARK-MATTER; GAS AB In modern hierarchical theories of structure formation, rich clusters of galaxies form at the vertices of a weblike distribution of matter, with filaments emanating from them to large distances and with smaller objects forming and draining in along these filaments. The amount of mass contained in structure near the cluster can be comparable to the collapsed mass of the cluster itself. As the lensing kernel is quite broad along the line of sight around cluster lenses with typical redshifts z(l) = 0.5, structures many megaparsecs parsecs away from the cluster are essentially at the same location as the cluster itself, when considering their effect on the cluster's weak lensing signal. We use large-scale numerical simulations of structure formation in a Lambda -dominated cold dark matter model to quantify the effect that large-scale structure near clusters has upon the cluster masses deduced from weak lensing analysis. A correction for the scatter in possible observed lensing masses should be included when interpreting mass functions from weak lensing surveys. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. RP Metzler, CA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM cmetzler@cfa.harvard.edu; mwhite@cfa.harvard.edu; cloken@ap.stmarys.ca RI White, Martin/I-3880-2015 OI White, Martin/0000-0001-9912-5070 NR 19 TC 80 Z9 80 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2001 VL 547 IS 2 BP 560 EP 573 DI 10.1086/318406 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 397ZF UT WOS:000166728300005 ER PT J AU di Matteo, T Carilli, CL Fabian, AC AF di Matteo, T Carilli, CL Fabian, AC TI Limits on the accretion rates onto massive black holes in nearby galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : individual (NGC 2300, NGC 1399, NGC 4278, NGC 4594); galaxies : nuclei; radio continuum : galaxies ID RADIO-CONTINUUM SOURCES; BRIGHT E/S0 GALAXIES; X-RAY; SYNCHROTRON-RADIATION; SPIRAL GALAXIES; LUMINOSITY; ELECTRONS; EMISSION; NUCLEI; CORES AB The radio emission from supermassive black holes in nearby early-type galaxies can be used to test possible explanations for their low luminosities. We calculate the expected contribution from thermal synchrotron emission from hot accretion flows to the high radio frequency observations of NGC 2300, NGC 1399, NGC 4278, and NGC 4594. We find that, in all cases, and in accordance with our previous findings, hot flows accreting close to their Bondi rates overestimate significantly the observed fluxes. This implies that simply assuming a low radiative efficiency for the accreting gas is not enough to explain their low luminosities. Smaller central densities and accretion rates, as expected in the presence of strong mass loss or convection in the flows, can help reconcile the models with observations. We also show that a significant contribution to the high-frequency radio spectra can be due to nonthermal synchrotron emission from the small-scale radio jets observed in these systems, allowing for even lower accretion rates in the inflows. We suggest that these outflows or jets may dump significant energy into the surrounding medium close to the accretion radius and thereby reduce the accretion rates onto these systems. We discuss the relationship between the radio flux and black hole mass for the observed sample and its potential importance for probing accretion models. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. RP di Matteo, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 46 TC 45 Z9 45 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2001 VL 547 IS 2 BP 731 EP 739 DI 10.1086/318405 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 397ZF UT WOS:000166728300019 ER PT J AU Dame, TM Hartmann, D Thaddeus, P AF Dame, TM Hartmann, D Thaddeus, P TI The milky way in molecular clouds: A new complete CO survey SO ASTROPHYSICAL JOURNAL LA English DT Review DE Galaxy : structure; ISM : clouds; ISM : molecules; radio lines : ISM; solar neighborhood; stars : formation ID HIGH GALACTIC LATITUDES; STAR-FORMING REGION; GAMMA-RAY EMISSION; ALL-SKY SURVEY; INFRARED-EMISSION; OUTER GALAXY; H-I; SUPERNOVA REMNANT; CEPHEUS FLARE; CIRRUS CLOUDS AB New large-scale CO surveys of the first and second Galactic quadrants and the nearby molecular cloud complexes in Orion and Taurus, obtained with the CfA 1.2 m telescope, have been combined with 31 other surveys obtained over the past two decades with that instrument and a similar telescope on Cerro Tololo in Chile, to produce a new composite CO survey of the entire Milky Way. The survey consists of 488,000 spectra that Nyquist or beamwidth sample the entire Galactic plane over a (1/8 degrees) strip 4 degrees -10 degrees wide in latitude, and beamwidth or sample nearly all large local clouds at higher latitudes. Compared with the previous composite CO survey of Dame et al. (1987), the new survey has 16 times more spectra, up to 3.4 times higher angular resolution, and up to 10 times higher sensitivity per unit solid angle. Each of the component surveys was integrated individually using clipping or moment masking to produce composite spatial and longitude-velocity maps of the Galaxy that display nearly all of the statistically significant emission in each survey but little noise. The composite maps provide detailed information on individual molecular clouds, suggest relationships between clouds and regions widely separated on the sky, and clearly display the main structural features of the molecular Galaxy. In addition, since the gas, dust, and Population I objects associated with molecular clouds contribute to the Galactic emission in every major wavelength band, the precise kinematic information provided by the present survey will form the foundation for many large-scale Galactic studies. A map of molecular column density predicted from complete and unbiased far-infrared and 21 cm surveys of the Galaxy was used both to determine the completeness of the present survey and to extrapolate it to the entire sky at \b\ < 32. The close agreement of the observed and predicted maps implies that only similar to2% of the total CO emission at \b\ < 32 lies outside our current sampling, mainly in the regions of Chamaeleon and the Gum Nebula. Taking into account this small amount of unobserved emission, the mean molecular column density decreases from similar to3 x 10(20) cm(2) at \b\ = 5 degrees to similar to0.1 x 10(20) cm(2) at \b\ = 30 degrees; this drop is similar to6 times steeper than would be expected from a plane-parallel layer, but is consistent with recent measurements of the mean molecular column density at higher latitudes. The ratio of the predicted molecular column density map to the observed CO intensity map provides a calibration of the CO-to-H-2 mass conversion factor X = NH2/W-CO. Out of the Galactic plane (\b\ > 5 degrees), X shows little systematic variation with latitude from a mean value of (1.8 +/- 0.3) x 10(20) cm(2) K-1 km(1) s. Given the large sky area and large quantity of CO data analyzed, we conclude that this is the most reliable measurement to date of the mean X value in the solar neighborhood. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tdame@cf.aharvard.edu; dap@strw.leidenuniv.nl; pthaddeus@cfa.harvard.edu NR 119 TC 1067 Z9 1073 U1 3 U2 16 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2001 VL 547 IS 2 BP 792 EP 813 DI 10.1086/318388 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 397ZF UT WOS:000166728300025 ER PT J AU Saito, M Kawabe, R Kitamura, Y Sunada, K AF Saito, M Kawabe, R Kitamura, Y Sunada, K TI An (HCO+)-C-13 survey for dense envelopes around low-mass embedded sources in Taurus SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM : clouds; ISM : molecules; stars : formation; stars : pre-main-sequence ID YOUNG STELLAR OBJECTS; L1551 IRS 5; MOLECULAR CLOUD; DARK CLOUDS; HL TAURI; CIRCUMPROTOSTELLAR ENVIRONMENTS; CONTINUUM OBSERVATIONS; PROTOSTELLAR COLLAPSE; INFALLING ENVELOPE; DETAILED STRUCTURE AB A dense gas survey was carried out toward 10 low-mass embedded young sources in Taurus with the Nobeyama Millimeter Array (NMA) to investigate protostellar evolution. All the sources were observed in the (HCO+)-C-13 (J = 1-0) line, a high-density tracer. Significant (HCO+)-C-13 emission (greater than or equal to4.5 sigma) was detected toward six of them. The (HCO+)-C-13 emission is distributed roughly perpendicular to the molecular outflow axes, indicating that the (HCO+)-C-13 line traces the dense envelopes associated with the central stars. The sizes and masses of the dense envelopes are estimated to be (1-7) x 10(3) AU and 0.01-0.2 M-., respectively. The 10 sources are divided into the following three classes based on their (HCO+)-C-13 intensities of the NMA maps, and their properties are studied using our own and other available data. Class A sources have (HCO+)-C-13 emission centered on the star with its elongation perpendicular to the molecular outflow axes. These sources also have dense outflowing gas and centrally condensed parent cores. Class B sources have (HCO+)-C-13 emission near the source positions and dense outflowing gas. The parent cores around class B sources, however, have a shallower density profile. Class C sources have neither (HCO+)-C-13 emission nor wing emission in dense gas tracers. From these properties, we conclude that low-mass protostars evolve from class A, B to C sources by dissipating their parent cloud cores, which is consistent with the widely accepted ideas of star formation. In addition, these observational data suggest that significant dispersion of a parent core by a molecular outflow and main accretion phase ends at the early protostellar phase. Six of the 10 sources are detected in continuum emission at 87 GHz. The intensities of the (HCO+)-C-13 emission do not correlate with the flux densities at 87 GHz. This is because our continuum maps trace compact disks on a 10(2) AU scale and not dense gas on a 10(3-4) AU scale. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. RP Saito, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM msaito@cfa.harvard.edu; kawabe@nro.nao.ac.jp; kitamura@pub.isas.ac.jp; sunada@nro.nao.ac.jp NR 65 TC 29 Z9 29 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2001 VL 547 IS 2 BP 840 EP 861 DI 10.1086/318383 PN 1 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 397ZF UT WOS:000166728300028 ER PT J AU Padoan, P Rosolowsky, EW Goodman, AA AF Padoan, P Rosolowsky, EW Goodman, AA TI The effects of noise and sampling on the spectral correlation function SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (Heiles's cloud 2); ISM : kinematics and dynamics; radio lines : ISM; turbulence ID STAR-FORMING REGIONS; MOLECULAR CLOUDS; INTERSTELLAR CLOUDS; FRACTAL STRUCTURE; SCALE STRUCTURE; DENSE CORES; DARK CLOUDS; TURBULENCE; TAURUS; STATISTICS AB The effects of noise and sampling on the spectral correlation function (SCF) introduced by Rosolowsky and coworkers are studied using observational data, numerical simulations of magneto-hydrodynamic turbulence, and simple models of Gaussian spectral line profiles. The most significant innovations of this paper are (1) the normalization of the SCF based on an analytic model for the effect of noise and (2) the computation of the SCF as a function of the spatial lag between spectra within a map. A new definition of the "quality" of a spectrum, Q, is introduced, which is correlated with the usual definition of signal-to-noise ratio. The prenormalization value of the SCF is a function of Q. We derive analytically the effect of noise on the SCF, and then normalize the SCF to its analytic approximation. By computing the dependence of the SCF on the spatial lag, S(0)(Deltar), we have been able to conclude the following : (1) S(0)(Deltar) is a power law, with slope a, in the range of scales l(i) < l < l(o). (2) The correlation outer scale, l(o), is determined by the size of the map, and no evidence for a true departure from selfl similarity on large scales has been found. (3) The correlation inner scale, l(i), is a true estimate of the smallest self-similar scale in a map. (4) The spectral slope, alpha, in a given region, is independent of velocity resolution (above a minimum resolution threshold), spatial resolution, and average spectrum quality. (5) Molecular transitions that trace higher gas density yield larger values of alpha (steeper slopes) than transitions tracing lower gas density. (6) Nyquist sampling, bad pixels in detector arrays, and referencesharing data acquisition need to be taken into account for a correct determination of the SCF at Deltar = 1. The value of alpha, however, can be computed correctly without a detailed knowledge of observational procedures. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Padoan, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ppadoan@cfa.harvard.edu; eros1@uclink.berkeley.edu; agoodman@cfa.harvard.edu RI Goodman, Alyssa/A-6007-2010; OI Goodman, Alyssa/0000-0003-1312-0477; Padoan, Paolo/0000-0002-5055-5800 NR 35 TC 22 Z9 22 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2001 VL 547 IS 2 BP 862 EP 871 DI 10.1086/318378 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 397ZF UT WOS:000166728300029 ER PT J AU Ghavamian, P Raymond, J Smith, RC Hartigan, P AF Ghavamian, P Raymond, J Smith, RC Hartigan, P TI Balmer-dominated spectra of nonradiative shocks in the Cygnus Loop, RCW 86, and Tycho supernova remnants SO ASTROPHYSICAL JOURNAL LA English DT Article DE radiative transfer; shock waves; supernova remnants ID LARGE MAGELLANIC CLOUD; X-RAY SPECTROSCOPY; ATOMIC-HYDROGEN; NOVA REMNANTS; OPTICAL-EMISSION; SN-1006; WAVE; ACCELERATION; IONIZATION; PROTONS AB We present an observational and theoretical study of the optical emission from nonradiative shocks in three supernova remnants: the Cygnus Loop, RCW 86, and Tycho. The spectra of these shocks are dominated by collisionally excited hydrogen Balmer lines, which have both a broad component caused by proton-neutral charge exchange and a narrow component caused by excitation of cold neutrals entering the shock. In each remnant, we have obtained the broad-to-narrow flux ratios of the H alpha and H beta lines and measured the H alpha broad component width. A new numerical shock code computes the broad and narrow Balmer line emission from nonradiative shocks in partially neutral gas. The Balmer line fluxes are sensitive to Lyman line trapping and the degree of electron-proton temperature equilibration. The code calculates the density, temperature, and size of the postshock ionization layer and uses a Monte Carlo simulation to compute narrow Balmer line enhancement from Lyman line trapping. The initial fraction of the shock energy allocated to the electrons and protons (the equilibration) is a free parameter. Our models show that variations in electron-proton temperature equilibration and Lyman line trapping can reproduce the observed range of broad-to-narrow ratios. The results give 80%-100% equilibration in nonradiative portions of the northeast Cygnus Loop (v(s) similar to 300 km s(-1)), 40%-50% equilibration in nonradiative portions of RCW 86 (v(s) similar to 600 km s(-1)), and less than or similar to 20% equilibration in Tycho (v(s) similar to 2000 km s(-1)). Our results suggest an inverse correlation between magnetosonic Mach number and equilibration in the observed remnants. C1 Rice Univ, Dept Space Phys & Astron, Houston, TX 77005 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ghavamian, P (reprint author), Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. NR 64 TC 125 Z9 127 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2001 VL 547 IS 2 BP 995 EP 1009 DI 10.1086/318408 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 397ZF UT WOS:000166728300041 ER PT J AU Finoguenov, A Jones, C AF Finoguenov, A Jones, C TI Chandra observation of M84, a radio lobe elliptical galaxy in the Virgo Cluster SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : abundances; galaxies : elliptical and lenticular, cD; galaxies : individual (NGC 4374) intergalactic medium; X-rays : galaxies ID RAY AB We analyzed a deep Chandra observation of M84, a bright elliptical galaxy in the core of the Virgo Cluster. We find that the spatial distribution of the soft X-ray emission is defined by the radio structure of the galaxy. In particular, we find two low-density regions associated with the radio lobes and surrounded by higher density X-ray filaments. In addition to a central active galactic nucleus (AGN) and a population of galactic sources, we find a diffuse hard source filling the central 10 kpc region. Since the morphology of the hard source appears round and is different from that seen in the radio or in soft X-rays, we propose that it is hot gas heated by the central AGN. Finally, we find that the central elemental abundance in the X-ray gas is comparable to that measured optically. C1 Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Finoguenov, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. NR 15 TC 82 Z9 82 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2001 VL 547 IS 2 BP L107 EP L110 DI 10.1086/318910 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398BA UT WOS:000166732800005 ER PT J AU Harnden, FR Adams, NR Damiani, F Drake, JJ Evans, NR Favata, F Flaccomio, E Freeman, P Jeffries, RD Kashyap, V Micela, G Patten, BM Pizzolato, N Schachter, JF Sciortino, S Stauffer, J Wolk, SJ Zombeck, MV AF Harnden, FR Adams, NR Damiani, F Drake, JJ Evans, NR Favata, F Flaccomio, E Freeman, P Jeffries, RD Kashyap, V Micela, G Patten, BM Pizzolato, N Schachter, JF Sciortino, S Stauffer, J Wolk, SJ Zombeck, MV TI Chandra observations of the open cluster NGC 2516 SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : individual (NGC 2516) stars : coronae; X-rays : stars ID COUNTING DETECTOR IMAGES; X-RAY SURVEY; N-LOG-S; WAVELET TRANSFORMS; ROSAT; DEEP AB Our analysis of Chandra X-Ray Observatory data for the open cluster NGC 2516, sometimes referred to as "the southern Pleiades," has yielded over 150 X-ray detections in both High-Resolution Camera and Advanced CCD Imaging Spectrometer images of the central region of the cluster. We identify some of the new X-ray sources with photometric cluster members and compare these new Chandra results with those of ROSAT. To date, 82 detected X-ray sources (42% of surveyed cluster members) are tentatively identified as cluster members. We also discuss the X-ray properties of late-type members in comparison with those of corresponding stellar types in the more metal-rich, approximately coeval Pleiades Cluster. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron Palermo Guiseppe S Vaiana, I-90134 Palermo, Italy. European Space Agcy, Div Astrophys, NL-2200 AG Noordwijk, Netherlands. Univ Keele, Dept Phys, Keele ST5 5BG, Staffs, England. Chase Secur, New York, NY 10017 USA. RP Harnden, FR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Flaccomio, Ettore/0000-0002-3638-5788; Micela, Giuseppina/0000-0002-9900-4751; Wolk, Scott/0000-0002-0826-9261; Damiani, Francesco/0000-0002-7065-3061 NR 16 TC 17 Z9 17 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2001 VL 547 IS 2 BP L141 EP L145 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398BA UT WOS:000166732800013 ER PT J AU Loeb, A Narayan, R Raymond, JC AF Loeb, A Narayan, R Raymond, JC TI Does the mass accretion rate depend on the radius of the accreting star? SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; stars : neutron; white dwarfs ID X-RAY TRANSIENTS; SS-CYGNI; CATACLYSMIC VARIABLES; DWARF NOVAE; U-GEMINORUM; BLACK-HOLES; DISK; QUIESCENCE; MODEL; OUTBURSTS AB In some circumstances, the mass accretion rate (M) over dot (*) onto a compact star may depend not only on external boundary conditions but also on the radius R-* of the accreting star. Writing the dependence as M-* proportional to R-*(p), we estimate p for transient binary systems in a quiescent state. We use the observed luminosities L of binary accreting white dwarfs (R-* similar to 10(9) cm) and neutron stars (R-* similar to 10(6) cm) under similar quiescent conditions and estimate M-* in each system through the relation L approximate to GM(*)M(*)/R-*, where M-* is the mass of the star. From the limited data available, we infer that p similar to 0.9 +/- 0.5 for quiescent binaries. This radial dependence is consistent with radiatively inefficient accretion flows that either are convective or lose mass via a wind. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Loeb, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 50 TC 7 Z9 7 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2001 VL 547 IS 2 BP L151 EP L154 DI 10.1086/318913 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398BA UT WOS:000166732800015 ER PT J AU Mao, S Loeb, A AF Mao, S Loeb, A TI Gravitational microlensing of gamma-ray burst afterglows by single and binary stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : general; cosmology : theory; gamma rays : bursts; gravitational lensing ID COSMOLOGICAL DENSITY; MACHO PROJECT; LIGHT CURVES; OBJECTS; FIREBALL; SPECTRA; EVENTS; SIZE AB We calculate the magnification light curves caused by stellar microlensing of gamma-ray burst (GRB) afterglows. A GRB source appears on the sky as a thin ring that expands faster than the speed of light and is maximally magnified as it crosses the lens caustics. While a single-star lens produces a single peak in the magnification light curve, binary-star lenses may produce multiple peaks. The shape of the magnification light curve provides invaluable information on the surface brightness distribution of the afterglow photosphere on submicroarcsecond scales. We find that all afterglows are likely to show variability at the level of a few percent about a year following the explosion, caused by stars that are separated by tens of Einstein radii from their line of sight. C1 Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mao, S (reprint author), Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. NR 29 TC 23 Z9 23 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2001 VL 547 IS 2 BP L97 EP L101 DI 10.1086/318912 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 398BA UT WOS:000166732800003 ER PT J AU Brown, CD Wise, MA AF Brown, CD Wise, MA TI Internal zonation and chemical evolution of the Black Mountain granitic pegmatite, Maine SO CANADIAN MINERALOGIST LA English DT Article DE granitic pegmatite; internal zonation; Black Mountain; Maine; tourmaline; spodumene; lepidolite; columbite; cassiterite AB The crystallization history of the Black Mountain granitic pegmatite. near Rumford, western Maine, is evaluated using compositions of rock-forming and accessory minerals. The pegmatite is strongly zoned; the zonation developed from the consolidation of a rare-element-enriched melt. Field and trace-element data show that the wall zone crystallized first from an initially B-enriched melt. Subsequent crystallization of three intermediate zones reflects changes in melt composition, which include a general decrease in levels of Mg, Ca, and Fe, and increases in levels of Be. Nb, Ta. Sn, and P. Significant enrichment in Li, Ph, Cs and F occurred during the latest stage of pegmatite crystallization prior to core development. Late albite-dominant units enriched in B, Nb > Ta, Sn and Zr replace primary zones; their chemical trends deviate from normal trends of fractionation (e.g., late enrichment in Pe). C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Brown, CD (reprint author), Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. NR 20 TC 13 Z9 13 U1 0 U2 2 PU MINERALOGICAL ASSOC CANADA PI NEPEAN PA CITYVIEW 78087, NEPEAN, ONTARIO K2G 5W2, CANADA SN 0008-4476 J9 CAN MINERAL JI Can. Mineral. PD FEB PY 2001 VL 39 BP 45 EP 55 DI 10.2113/gscanmin.39.1.45 PN 1 PG 11 WC Mineralogy SC Mineralogy GA 423WG UT WOS:000168200300004 ER PT J AU Greenberg, R Gonzales, CE Bichier, P Reitsma, R AF Greenberg, R Gonzales, CE Bichier, P Reitsma, R TI Nonbreeding habitat selection and foraging behavior of the Black-throated Green Warbler complex in southeastern Mexico SO CONDOR LA English DT Article DE Dendroica; foraging ecology; Neotropical migrants; Parulidae; winter ecology ID TIME AB We studied the ecological distribution and foraging behavior of three species in the Black-throated Green Warbler (Dendroica virens) species group in the Eastern Highlands of Chiapas, Mexico. The three species. Black-throated Green, Hermit (D. occidentalis) and Townsend's (D. townsendi) Warblers are largely allopatric on the breeding grounds and variably sympatric during the winter. We surveyed the composition of 166 mixed-species flocks and recorded habitat variables associated with the flock location along an elevational transect. We found that Black-throated Green and Townsend's Warblers segregated by altitude, whereas Hermit Warbler overlapped extensively with both other species. Even though Townsend's and Hermit Warblers co-occurred commonly in the same Rocks, the latter showed strong selective use of pine trees and the former showed weaker selectivity of oak trees. Black-throated Green Warbler showed no tree-type selection. The combined differences in elevational distribution and tree-type use resulted in very low ecological overlap for the three species. The Black-throated Green Warbler was the most distinct in its foraging behavior, occurring more often in the outer and upper branches of trees, and using hanging, aerial, and hovering maneuvers more than its congeners. In addition, it showed a higher movement frequency and a lower rate of between-branch flights. The Black-throated Green Warbler also is the most morphologically distinct as a result of its overall smaller body size, which is consistent for the trend towards larger body size in more conifer-specialized species in this genus. We propose that as new breeding populations were founded, and speciation occurred, individuals of the more derived species occupied decreasingly productive winter habitats. C1 Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. RP Greenberg, R (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. NR 27 TC 2 Z9 2 U1 0 U2 4 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 J9 CONDOR JI Condor PD FEB PY 2001 VL 103 IS 1 BP 31 EP 37 DI 10.1650/0010-5422(2001)103[0031:NHSAFB]2.0.CO;2 PG 7 WC Ornithology SC Zoology GA 400NJ UT WOS:000166877800004 ER PT J AU Taylor, SS Leonard, ML Boness, DJ AF Taylor, SS Leonard, ML Boness, DJ TI Aggressive nest intrusions by male Humboldt Penguins SO CONDOR LA English DT Article DE Humboldt Penguin; infanticide; mate usurpation; mating strategy; skewed sex ratio; Spheniscus humboldti ID POPULATION AB During observations at a breeding colony of Humboldt Penguins (Spheniscus humboldti), we noted five male penguins enter nests occupied by breeding pairs and engage in aggressive interactions with the resident adult. These nest intrusions resulted in egg loss or infanticide, and accounted for 11.1% of breeding failure in the colony. Two intruder males ultimately mated with respective resident females. This behavior had not been observed previously in Humboldt Penguins and we suggest that it may occur when males are unable to obtain mates through advertising at the nest. Intrusion behavior may slow down population recovery in this endangered species. C1 Dalhousie Univ, Dept Biol, Halifax, NS B3H 4J1, Canada. Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. RP Taylor, SS (reprint author), Dalhousie Univ, Dept Biol, Halifax, NS B3H 4J1, Canada. NR 16 TC 12 Z9 12 U1 4 U2 13 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 J9 CONDOR JI Condor PD FEB PY 2001 VL 103 IS 1 BP 162 EP 165 DI 10.1650/0010-5422(2001)103[0162:ANIBMH]2.0.CO;2 PG 4 WC Ornithology SC Zoology GA 400NJ UT WOS:000166877800019 ER PT J AU Laurance, WF AF Laurance, WF TI Tropical logging and human invasions SO CONSERVATION BIOLOGY LA English DT Letter ID AMAZONIAN FORESTS; CRISIS; FIRE C1 Smithsonian Trop Res Inst, Balboa, Panama. Natl Inst Amazonian Res, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. RI Laurance, William/B-2709-2012 NR 16 TC 31 Z9 34 U1 1 U2 7 PU BLACKWELL SCIENCE INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 2001 VL 15 IS 1 BP 4 EP 5 DI 10.1046/j.1523-1739.2001.00_11-2.x PG 2 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 405QK UT WOS:000167170400003 ER PT J AU Small, AM Adey, WH AF Small, AM Adey, WH TI Reef corals, zooxanthellae and free-living algae, a microcosm study that demonstrates synergy between calcification and primary production SO ECOLOGICAL ENGINEERING LA English DT Article DE microcosm; coral reefs; calcification; photosynthesis; algae; corals; synergy ID SEA CO2 FLUXES; FRENCH-POLYNESIA; COMMUNITY METABOLISM; CARBON-DIOXIDE; ECOSYSTEMS; NUTRIENT; DYNAMICS; MOOREA AB A mature, high-biodiversity coral reef microcosm and its chambered subsets were used to examine the relationship between calcification and photosynthesis and its most critical biotic components. Whole ecosystem calcification at 4.0 +/- 0.2 kg (40 +/- 2 mol) CaCO3 m(-2) year(-1) is related to its primary components (stony coral 17.6%, Halimeda 7.4%, Tridacna 9.0%, algal turf, coralline and foraminifera 29.4%, and miscellaneous invertebrates 36%). Through analysis of the microcosm's daily carbonate system, it is demonstrated that bicarbonate ion, not carbonate ion, is the principal component of total alkalinity reduction in the water column (thus, bicarbonate ion is the principal measured component of calcification as normally measured on reef transects). While chamber-isolated free-living algae remove carbon dioxide, and raise pH and carbonate ion equivalent to that in the microcosm as a whole, no total alkalinity reduction (calcification) occurs. On the other hand, chamber isolated stony corals remove considerable bicarbonate, with very little pH or carbonate ion elevation: Combining the non-calcifying free-living macroalgae Chondria with stony corals in chamber subsets, it is possible to remove more carbon dioxide (elevating pH) and thereby increase coral calcification rates by 60 and 120% above zooxanthellae-mediated rates to 20.6 kg (206 mol) and 18.5 kg (185 mol) CaCO3 m(-2) year(-1) for Acropora and Montipora, respectively. These findings, which support the McConnaughey and Whelan hypothesis of bicarbonate ion neutralization in coral calcification, are easily demonstrated in the controlled microcosm environment. (C) 2001 Elsevier Science B.V. All rights reserved. C1 Smithsonian Inst, Marine Syst Lab, Washington, DC 20560 USA. RP Adey, WH (reprint author), Smithsonian Inst, Marine Syst Lab, NHB E-117,MRC 164, Washington, DC 20560 USA. NR 41 TC 12 Z9 13 U1 2 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0925-8574 J9 ECOL ENG JI Ecol. Eng. PD FEB PY 2001 VL 16 IS 4 BP 443 EP 457 DI 10.1016/S0925-8574(00)00066-5 PG 15 WC Ecology; Engineering, Environmental; Environmental Sciences SC Environmental Sciences & Ecology; Engineering GA 397MR UT WOS:000166699900001 ER PT J AU Pandolfi, JM Jackson, JBC AF Pandolfi, JM Jackson, JBC TI Community structure of Pleistocene coral reefs of Curacao, Netherlands Antilles SO ECOLOGICAL MONOGRAPHS LA English DT Review DE Caribbean; community ecology; community structure; coral; coral reefs; paleoecology; Pleistocene; Quaternary ID GREAT-BARRIER-REEF; PATCH REEFS; MONTASTRAEA-ANNULARIS; TEMPORAL VARIABILITY; HERMATYPIC CORALS; DEATH ASSEMBLAGES; SPECIES RICHNESS; DEPTH GRADIENTS; HUON PENINSULA; LONG-TERM AB The Quaternary fossil record of living coral reefs is fundamental for understanding modern ecological patterns. Living reefs generally accumulate in place, so fossil reefs record a history of their former biological inhabitants and physical environments. Reef corals record their ecological history especially well because they form large, resistant skeletons, which can be identified to species. Thus, presence-absence and relative abundance data can be obtained with a high degree of confidence. Moreover, potential effects of humans on reef ecology were absent or insignificant on most reefs until the last few hundred years, so that it is possible to analyze "natural" distribution patterns before intense human disturbance began. We characterized Pleistocene reef coral assemblages from Curacao, Netherlands Antilles, Caribbean Sea, focusing on predictability in species abundance patterns from different reef environments over broad spatial scales. Our data set is composed of >2 km of surveyed Quaternary reef. Taxonomic composition showed consistent differences between environments and along secondary environmental gradients within environments. Within environments, taxonomic composition of communities was markedly similar indicating nonrandom species associations and communities composed of species occurring in characteristic abundances. This community similarity was maintained with little change over a 40-km distance. The nonrandom patterns in species abundances were similar to those found in the Caribbean before the effects of extensive anthropogenic degradation of reefs in the late 1970s and early 1980s. The high degree of order observed in species abundance patterns of fossil reef coral communities on a scale of tens of kilometers contrasts markedly with patterns observed in previous small-scale studies of modern reefs. Dominance of Acropora palmata in the reef crest zone and patterns of overlap and nonoverlap of species in the Montastraea ''annularis'' sibling species complex highlight the tendency for distribution and abundance patterns of Pleistocene corals to reflect environmental preferences at multiple spatial scales. Wave energy is probably the most important physical environmental variable structuring these coral communities. The strong similarity between ancient and pre-1980s Caribbean reefs and the nonrandom distribution of coral species in space and time indicate that recent variability noted at much smaller time scales may be due to either unprecedented anthropogenic influences on reefs or fundamentally different patterns at varying spatio-temporal scales. C1 Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa, Panama. RP Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC-121, Washington, DC 20560 USA. RI Pandolfi, John/A-3121-2009 OI Pandolfi, John/0000-0003-3047-6694 NR 151 TC 60 Z9 65 U1 1 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9615 EI 1557-7015 J9 ECOL MONOGR JI Ecol. Monogr. PD FEB PY 2001 VL 71 IS 1 BP 49 EP 67 DI 10.1890/0012-9615(2001)071[0049:CSOPCR]2.0.CO;2 PG 19 WC Ecology SC Environmental Sciences & Ecology GA 401EH UT WOS:000166914000003 ER PT J AU Rohwer, S Bermingham, E Wood, C AF Rohwer, S Bermingham, E Wood, C TI Plumage and mitochondrial DNA haplotype variation across a moving hybrid zone SO EVOLUTION LA English DT Article DE character transition; cytonuclear linkage; Dendroica occidentalis; Dendroica townsendi; hybrid zone; mitochondrial DNA; phylogeography; sexual selection ID GENE FLOW; DENDROICA WARBLERS; TOWNSENDS WARBLERS; HALDANES RULE; SPECIATION; DIFFERENTIATION; ADAPTATION; COMPLEX; HERMIT AB We analyze variation in phenotypes and mitochondrial DNA (mtDNA) haplotypes over the breeding ranges of hermit and Townsend's warblers and across two of their three hybrid zones. Within these two hybrid zones, we demonstrate that the placement, shape, and width of transitions in seven plumage characters are remarkably similar, suggesting that a balance between dispersal and sexual selection keeps these hybrid zones narrow. A consistent asymmetry in these character transition curves suggests that Townsend's warblers have a selective advantage over hermit warblers, which is presumably due to the aggressive superiority of Townsend's over hermit males (Pearson and Rohwer 2000). An association between plumage and mtDNA haplotypes shows that pure Townsend's warblers, but not pure hermit warblers, immigrate into these hybrid zones, further supporting the competitive superiority of Townsend's warblers over hermit warblers. The mitochondrial haplotype transitions across these hybrid zones are much wider than the phenotypic transitions and provide no indication that the mtDNA haplotypes representing these two warblers are selectively maintained. More importantly, the phenotypically pure populations of Townsend's warblers throughout a 2000-km coastal strip north of the Washington hybrid zones contain a preponderance of hermit warbler mtDNA haplotypes. This result suggests massive movement of the hybrid zone between these warblers during the 5000 years since their most recent interglacial contact. We develop a model to explain the phenotypic and genetic divergence between these warblers and the evolution of their dramatic differences in aggressiveness; we also show how differences in male aggression, in combination with biased pairing patterns, can explain the haplotype footprint recording the historical movement of this hybrid zone. C1 Univ Washington, Burke Museum, Seattle, WA 98195 USA. Univ Washington, Dept Zool, Seattle, WA 98195 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Rohwer, S (reprint author), Univ Washington, Burke Museum, Box 353010, Seattle, WA 98195 USA. NR 58 TC 114 Z9 118 U1 4 U2 24 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD FEB PY 2001 VL 55 IS 2 BP 405 EP 422 PG 18 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 412KD UT WOS:000167552800016 PM 11308096 ER PT J AU Wang, JH Davis, AM Clayton, RN Mayeda, TK Hashimoto, A AF Wang, JH Davis, AM Clayton, RN Mayeda, TK Hashimoto, A TI Chemical and isotopic fractionation during the evaporation of the FeO-MgO-SiO2-CaO-Al2O3-TiO2 rare earth element melt system SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID EARLY SOLAR NEBULA; UNUSUAL ALLENDE INCLUSION; REFRACTORY INCLUSIONS; HIBONITE INCLUSIONS; ANOMALIES; CONDENSATION; MAGNESIUM; HAL; METEORITES; FORSTERITE AB A synthetic material with solar elemental proportions of iron, magnesium, silicon. titanium, calcium, and aluminum oxides and doped with rare earth elements was evaporated in a vacuum furnace at 1800 and 2000 degreesC for different durations to study its chemical and isotopic evolution during the evaporation process. It is demonstrated that kinetic evaporation of solar composition material can produce residues of calcium-, aluminum-rich inclusion bulk chemistry. The evaporation sequence of the main constituents in this solar composition material is iron > silicon approximate to magnesium > titanium, Calcium and aluminum remain unevaporated after evaporation of 95% of the solar composition material. The chemical fractionation between the gas and condensed phase is a function not only of temperature and pressure, but also of the hulk chemical composition of the condensed phase. During the evaporation process, cerium is almost as volatile as iron. The 2,000-fold cerium depletion found in some refractory inclusions in carbonaceous chondrites was reproduced in the evaporation experiment and can be readily explained as a result of evaporation of preexisting meteoritic material. Kinetic isotopic fractionation of magnesium, oxygen, and silicon follows the Rayleigh distillation law during the laboratory evaporation of synthetic solar composition material. This implies that the residue is well mixed during the evaporation process and that the evaporation kinetic processes (both chemical and isotopic) are surface reaction-controlled. The isotopic mass fractionation factors are lower than those predicted from theoretical calculations by using the square root of mass ratios of likely evaporating species. Thus, the surface reaction is more complicated than decomposition into single gas species of each element. Copyright (C) 2001 Elsevier Science Ltd. C1 Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Univ Chicago, Dept Chem, Chicago, IL 60637 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Davis, AM (reprint author), Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA. RI Wang, Jianhua/D-6500-2011; OI Wang, Jianhua/0000-0002-7671-2413; Davis, Andrew/0000-0001-7955-6236 NR 63 TC 80 Z9 82 U1 6 U2 19 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD FEB PY 2001 VL 65 IS 3 BP 479 EP 494 DI 10.1016/S0016-7037(00)00529-9 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 399AP UT WOS:000166788900011 ER PT J AU Manning, RB Camp, DK AF Manning, RB Camp, DK TI A new genus of stomatopod from the Caribbean Sea (Stomatopoda : Squillidae) SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article AB A new genus, Humesosquilla, is recognized for Squilla decimdentata Manning, 1970. It can be distinguished from all recognized species of Squilla sensu Manning, 1969, sharing a single lateral process of the fifth thoracic somite by the presence of 10-11 teeth on the dactylus of the raptorial claw. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Camp, DK (reprint author), 11990 68th Ave N, Seminole, FL 33772 USA. NR 14 TC 1 Z9 2 U1 1 U2 1 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD FEB PY 2001 VL 21 IS 1 BP 202 EP 204 DI 10.1651/0278-0372(2001)021[0202:ANGOSF]2.0.CO;2 PG 3 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 404DR UT WOS:000167082600013 ER PT J AU Eberhard, WG AF Eberhard, WG TI Trolling for water striders: active searching for prey and the evolution of reduced webs in the spider Wendilgarda sp (Araneae, Theridiosomatidae) SO JOURNAL OF NATURAL HISTORY LA English DT Article DE spiders; webs; construction behaviour; Wendilgarda; behavioural evolution ID PHYLOGENY; CONSTRUCTION AB Wendilgarda sp. builds unusually simple webs attached to the surface of water. The simplest design consists of a single vertical line with sticky material near the bottom that is attached at the top to a single horizontal line and at the bottom to the water surface. The spider usually sits immobile waiting for prey as the sticky line skates erratically across the surface of the water, but some spiders actively dragged their webs back and forth across the water. The web's simplicity is apparently derived with respect to the webs of other Wendilgarda species, as spiders sometimes made more complex webs similar to typical Wendilgarda webs. The simplicity of W. sp. webs may be causally related to two other unusual traits: extreme variability in web design and construction behaviour and web manipulation behaviour; and construction of prey capture webs with sticky lines by mature males, confirmed here for the first time in a confirmed member of an orb-weaving family. Some behavioural innovations in Wendilgarda, such as the attachment of a short segment of non-sticky silk to the water surface just prior to laying each segment of sticky line, may represent blocks of behaviour that have been shifted temporally in the web construction sequence. C1 Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, San Jose, Costa Rica. NR 36 TC 13 Z9 18 U1 0 U2 1 PU TAYLOR & FRANCIS LTD PI LONDON PA 11 NEW FETTER LANE, LONDON EC4P 4EE, ENGLAND SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PD FEB PY 2001 VL 35 IS 2 BP 229 EP 251 DI 10.1080/00222930150215350 PG 23 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 395FH UT WOS:000166568900007 ER PT J AU Berntson, EA Bayer, FM McArthur, AG France, SC AF Berntson, EA Bayer, FM McArthur, AG France, SC TI Phylogenetic relationships within the Octocorallia (Cnidaria : Anthozoa) based on nuclear 18S rRNA sequences SO MARINE BIOLOGY LA English DT Article ID MAXIMUM-LIKELIHOOD; DNA; ORDER AB We determined the nuclear 18S rRNA sequences for 41 species of octocorals and used these to address the validity of the historical ordinal divisions and the current subordinal divisions within the subclass Octocorallia. We also explored the phylogenetic affinities of the species Dendrobrachia paucispina, which was originally classified in the order Antipatharia (subclass Ceriantipatharia) although polyp structure indicates it belongs in the subclass Octocorallia. Trees constructed using maximum likelihood techniques are incongruent with the current and historical taxonomy of the Octocorallia. There appeared to be three major clades of octocorals. The first clade included most, but not all, pennatulaceans as a monophyletic group. The second clade contained 21 species, representing all major octocoral groups other than pennatulaceans. The third clade contained members from three suborders of the Alcyonacea and one member of the Pennatulacea. These data could not be used to distinguish the branching order of the three major clades. The species D. paucispina had a close affinity with the genera Corallium and Paragorgia (Alcyonacea: Scleraxonia), although its morphology suggests it is more similar to the genus Chrysogorgia (Alcyonacea: Calcaxonia). The morphological character of dimorphism (the presence of both autozooids and siphonozooids within a single colony) corresponded loosely with the topology of the most likely trees, and a single origin of dimorphism could not be rejected. Despite sampling from the majority of families within the Octocorallia, many of the relationships within this group remain ambiguous. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20560 USA. Marine Biol Lab, Josephine Bay Paul Ctr, Woods Hole, MA 02543 USA. Coll Charleston, Dept Biol, Charleston, SC 29424 USA. Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA. RP Berntson, EA (reprint author), Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Conservat Biol Div, 2725 Montlake Blvd E, Seattle, WA 98112 USA. NR 40 TC 52 Z9 60 U1 1 U2 3 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD FEB PY 2001 VL 138 IS 2 BP 235 EP 246 DI 10.1007/s002270000457 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 406BB UT WOS:000167194100002 ER PT J AU Burbine, TH Binzel, RP Bus, SJ Clark, BE AF Burbine, TH Binzel, RP Bus, SJ Clark, BE TI K asteroids and CO3/CV3 chondrites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CO3 CARBONACEOUS CHONDRITE; MEAN MOTION RESONANCES; SPECTRAL CHARACTERISTICS; EOS FAMILY; S-TYPE; PHYLLOSILICATES; MATRIX; CV AB Reflectance spectra from 0.44 to 1.65 mum were obtained for three K asteroids. These objects all have spectra consistent with olivine-dominated assemblages whose absorption bands have been suppressed by opaques. The two observed Eos family members (221 Eos and 653 Berenike) are spectral analogs to the CO3 chondrite Warrenton. The other observed object (599 Luisa) is a spectral analog for CV3 chondrite Mokoia. These asteroids are all located near meteorite-supplying resonances with the Eos family cut by the 9:4 resonance and Luisa is found near the 5:2 resonance. However, K asteroids have been identified throughout the main belt so it is difficult to rule out other possible parent bodies for the CO3 and CV3 chondrites. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. RP Burbine, TH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. NR 38 TC 23 Z9 23 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 0026-1114 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD FEB PY 2001 VL 36 IS 2 BP 245 EP 253 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 414EK UT WOS:000167652800008 ER PT J AU Sivasundar, A Bermingham, E Orti, G AF Sivasundar, A Bermingham, E Orti, G TI Population structure and biogeography of migratory freshwater fishes (Prochilodus : Characiformes) in major South American rivers SO MOLECULAR ECOLOGY LA English DT Article DE freshwater fishes; mitochondrial DNA; Parana Basin; phylogeography; Prochilodus ID MAXIMUM-LIKELIHOOD-ESTIMATION; DNA-SEQUENCE DATA; MITOCHONDRIAL-DNA; PARANA RIVER; GEOGRAPHICAL-DISTRIBUTION; CLADISTIC-ANALYSIS; WATER FISHES; GENE FLOW; EVOLUTION; SUBSTITUTION AB Mitochondrial DNA (mtDNA) sequences were used to infer the phylogenetic relationships of Prochilodus species in the Parana, Amazonas, Orinoco, and Magdalena basins. Sequences of ATPase subunits 6 and 8 (total 840 bp) were obtained for 21 Prochilodus specimens from the four river systems. Using Semaprochilodus as an outgroup, phylogenetic analyses showed that: (i) each river basin contains a monophyletic group of mtDNA lineages; and (ii) the branching order places Magdalena in a basal position with subsequent branching of Orinoco, Amazon and Parana. The mitochondrial control region was sequenced for 26 P. lineatus (from the Parana basin) and six other Prochilodus specimens from the Magdalena, Orinoco and Amazon. All 26 control region haplotypes were unique with sequence divergence ranging from 0.3 to 3.6%. The control region phylogeny is well resolved but phylogenetic structure is not associated with geography. For example, mtDNA haplotypes from the upper Parana (Mogui Guassu) and the upper Bermejo, separated by at least 2600 km, have close genealogical ties. Phylogeographic analyses, including nested clads analysis, suggest high levels of gene flow within this basin. C1 Univ Nebraska, Sch Biol Sci, Lincoln, NE 68588 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Orti, G (reprint author), Univ Nebraska, Sch Biol Sci, Lincoln, NE 68588 USA. NR 56 TC 139 Z9 147 U1 1 U2 20 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD FEB PY 2001 VL 10 IS 2 BP 407 EP 417 DI 10.1046/j.1365-294x.2001.01194.x PG 11 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 416KJ UT WOS:000167779400012 PM 11298955 ER PT J AU White, M AF White, M TI The redshift-space power spectrum in the halo model SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmology : theory; large-scale structure of Universe ID LARGE-SCALE STRUCTURE; DISTORTIONS; GALAXIES AB Recently there has been a lot of attention focused on a virialized halo-based approach to understanding the properties of the matter and galaxy power spectrum. We show that this model allows a natural treatment of the large- and small-scale redshift-space distortions, which we develop here, which extends the pedagogical value of the approach. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP White, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI White, Martin/I-3880-2015 OI White, Martin/0000-0001-9912-5070 NR 19 TC 64 Z9 64 U1 0 U2 3 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2001 VL 321 IS 1 BP 1 EP 3 DI 10.1046/j.1365-8711.2001.03956.x PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 405HD UT WOS:000167153200006 ER PT J AU Dutta, CM Nordlander, P Kimura, M Dalgarno, A AF Dutta, CM Nordlander, P Kimura, M Dalgarno, A TI Charge-transfer cross sections in collisions of ground state Na atoms with H+ at low-eV collision energies SO PHYSICAL REVIEW A LA English DT Article ID SMALL-SCALE STRUCTURE; ELECTRON-CAPTURE; EXCHANGE COLLISIONS; TARGET EXCITATION; HYDROGEN; PROTONS; IONS AB Cross sections for nonradiative charge transfer in H+ +Na(3s) collisions at energies less than or equal to 40 eV have been calculated using a fully quantum-mechanical approach. The calculated cross sections agree well with the experimental data in the entire energy range, but do not agree with ether calculations at low energies. We discuss possible causes of this difference. Using the calculated cross sections, the rate coefficients at temperatures below 20 000 K have been calculated, and compared with those of other theoretical calculations. C1 Dept Phys, Houston, TX 77251 USA. Rice Univ, Rice Quantum Inst, Houston, TX 77251 USA. Yamaguchi Univ, Grad Sch Sci & Engn, Ube, Yamaguchi 755, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dutta, CM (reprint author), Dept Phys, Houston, TX 77251 USA. RI Nordlander, Peter/A-2560-2008 OI Nordlander, Peter/0000-0002-1633-2937 NR 25 TC 5 Z9 5 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD FEB PY 2001 VL 63 IS 2 AR 022709 DI 10.1103/PhysRevA.63.022709 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 400JF UT WOS:000166867900059 ER PT J AU Garay, LJ Anglin, JR Cirac, JI Zoller, P AF Garay, LJ Anglin, JR Cirac, JI Zoller, P TI Sonic black holes in dilute Bose-Einstein condensates SO PHYSICAL REVIEW A LA English DT Article ID HAWKING RADIATION; DARK SOLITONS; MOVING-MEDIA; ATOM LASER; EVAPORATION; HORIZONS; ANALOG; GAS; VORTICES; CREATION AB The sonic analog of a gravitational black hole in dilute-gas Bose-Einstein condensates is investigated. It is shown that there exist both dynamically stable and unstable configurations which, in the hydrodynamic limit, exhibit behaviors completely analogous to that of gravitational black holes. The dynamical instabilities involve the creation of quasiparticle pairs in positive and negative energy states. We illustrate these features in two qualitatively different one-dimensional models, namely, a long, thin condensate with an outcoupler laser beam providing an "atom sink" and a tight ring-shaped condensate. We also simulate the creation of a stable sonic black hole by solving the Gross-Pitaevskii equation numerically for a condensate subject to a trapping potential which is adiabatically deformed. A sonic black hole could, in this way, be created experimentally with state-of-the-art or planned technology. C1 Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. CSIC, Inst Matemat & Fis Fundamental, E-28006 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02135 USA. RP Univ Innsbruck, Inst Theoret Phys, Technikerstr 25, A-6020 Innsbruck, Austria. RI Garay, Luis J./C-2544-2013; Zoller, Peter/O-1639-2014 OI Garay, Luis J./0000-0002-3943-7782; Zoller, Peter/0000-0003-4014-1505 NR 42 TC 127 Z9 128 U1 0 U2 7 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD FEB PY 2001 VL 63 IS 2 AR 023611 DI 10.1103/PhysRevA.63.023611 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 400JF UT WOS:000166867900093 ER PT J AU Kharchenko, V Dalgarno, A AF Kharchenko, V Dalgarno, A TI Refractive index for matter waves in ultracold gases SO PHYSICAL REVIEW A LA English DT Article ID INTERFEROMETRY; SCATTERING; MOLECULES; OPTICS AB An analytical expression for the refractive index of atomic and molecular matter waves in ultracold,oases is obtained. Asymptotic formulas for the refractive index are derived for high and low projectile velocities, and intermediate velocities are investigated with the eikonal approximation. The real and imaginary parts of the matter wave refractive index are expressed via the complex scattering length of elastic and superelastic collisions. It is shown that superelastic collisions dramatically influence the low-energy behavior of the refractive index. A discussion is given of proposed measurements of the real and imaginary parts of the scattering length using the interferometry of slow de Broglie waves. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Kharchenko, V (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. NR 18 TC 12 Z9 12 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD FEB PY 2001 VL 63 IS 2 AR 023615 DI 10.1103/PhysRevA.63.023615 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 400JF UT WOS:000166867900097 ER PT J AU Menotti, C Anglin, JR Cirac, JI Zoller, P AF Menotti, C Anglin, JR Cirac, JI Zoller, P TI Dynamic splitting of a Bose-Einstein condensate SO PHYSICAL REVIEW A LA English DT Article ID QUANTUM PHASE DIFFUSION; FLUCTUATIONS; EXCITATIONS; REVIVALS AB We study the dynamic process of splitting a condensate by raising a potential barrier in the center of a harmonic trap. We use a two-mode model to describe the phase coherence between the two halves of the condensate. Furthermore, we explicitly consider the spatial dependence of the mode funtions, which varies depending an the potential barrier. This allows us to get the tunneling coupling between the two wells and the on-site energy as a function of the barrier height. Moreover, we can get some insight into the collective modes that are excited by raising the barrier. We describe the internal and external degrees of freedom by variational ansatz. We distinguish the possible regimes as a function of the characteristic parameters of the problem and identify the adiabaticity conditions. C1 Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. Scuola Normale Super Pisa, I-56126 Pisa, Italy. Univ Pisa, Dipartimento Fis, Unita INFM, I-56126 Pisa, Italy. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02135 USA. RP Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. RI Zoller, Peter/O-1639-2014 OI Zoller, Peter/0000-0003-4014-1505 NR 30 TC 75 Z9 76 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD FEB PY 2001 VL 63 IS 2 AR 023601 DI 10.1103/PhysRevA.63.023601 PG 15 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 400JF UT WOS:000166867900083 ER PT J AU Wargelin, BJ Kahn, SM Beiersdorfer, P AF Wargelin, BJ Kahn, SM Beiersdorfer, P TI Dielectronic satellite contributions to NeVIII and NeIX K-shell spectra SO PHYSICAL REVIEW A LA English DT Article ID BEAM ION-TRAP; HE-LIKE IONS; ELECTRON-IMPACT; CROSS-SECTIONS; POLARIZATION; LINES; EXCITATION; EMISSION; LIFETIME; LEVEL AB K alpha spectra of heliumlike neon and associated lithiumlike, berylliumlike, and boronlike satellite line emission have been observed with a high-resolution crystal spectrometer on the Lawrence Livermore Electron Beam Ion Trap. The KLL dielectronic recombination satellites were resolved from their He-like parent lines in electron energy space, and their wavelengths and resonance strengths measured. The wavelength measurements achieved a typical accuracy of a few m Angstrom, with two measurements accurate to better than one part in 10 000. By normalizing to the He-like resonance line, w, we measure Li-like satellite resonance strengths that are 10% to 46% lower than predicted by theoretical models. The wavelengths and relative strengths of Be-like KLL satellites were also measured, and absolute strengths were obtained by normalizing to the collisionally excited Li-like qr satellite blend. C1 Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 31 TC 19 Z9 20 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD FEB PY 2001 VL 63 IS 2 AR 022710 DI 10.1103/PhysRevA.63.022710 PG 11 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 400JF UT WOS:000166867900060 ER PT J AU Barth, C Krause, GH Winter, K AF Barth, C Krause, GH Winter, K TI Responses of photosystem I compared with photosystem II to high-light stress in tropical shade and sun leaves SO PLANT CELL AND ENVIRONMENT LA English DT Article DE carotenoids; chlorophyll fluorescence; P700 absorbance change; photo-inhibition; xanthophyll cycle ID XANTHOPHYLL-CYCLE ACTIVITY; CUCUMIS-SATIVUS L; HIGHER-PLANTS; CHLOROPHYLL FLUORESCENCE; ISOLATED-CHLOROPLASTS; SPINACIA-OLERACEA; LOW-TEMPERATURES; PEA LEAVES; D1 PROTEIN; PHOTOINHIBITION AB Sun and shade leaves of several plant species from a neotropical forest were exposed to excessive light to evaluate the responses of photosystem I in comparison to those of photosystem II. Potential photosystem I activity was determined by means of the maximum P700 absorbance change around 810 nm (DeltaA(810max)) in saturating far-red light. Leaf absorbance changes in dependence of increasing far-red light fluence rates were used to calculate a 'saturation constant', K-s, representing the far-red irradiance at which half of the maximal absorbance change (DeltaA(810max)/2) was reached in the steady state. Photosystem II efficiency was assessed by measuring the ratio of variable to maximum chlorophyll fluorescence, F-v/F-m, in dark-adapted leaf samples. Strong illumination caused a high degree of photo-inhibition of photosystem II in all leaves, particularly in shade leaves. Exposure to 1800-2000 mu mol photons m(-2) s(-1) for 75 min did not substantially affect the potential activity of photosystem I in all species tested, but caused a more than 40-fold increase of K-s in shade leaves, and a three-fold increase of K-s in sun leaves. The increase in K-s was reversible during recovery under low light, and the recovery process was much faster in sun than in shade leaves. The novel effect of high-light stress on the light saturation of P700 oxidation described here may represent a complex reversible mechanism within photosystem I that regulates light-energy dissipation and thus protects photosystem I from photo-oxidative damage. Moreover, we show that under high-light stress a high proportion of P700 accumulates in the oxidized state, P700(+). Presumably, conversion of excitation energy to heat by this cation radical may efficiently contribute to photoprotection. C1 Univ Dusseldorf, Inst Plant Biochem, D-40225 Dusseldorf, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Krause, GH (reprint author), Univ Dusseldorf, Inst Plant Biochem, Univ Str 1, D-40225 Dusseldorf, Germany. NR 57 TC 49 Z9 63 U1 1 U2 16 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 0140-7791 J9 PLANT CELL ENVIRON JI Plant Cell Environ. PD FEB PY 2001 VL 24 IS 2 BP 163 EP 176 DI 10.1046/j.1365-3040.2001.00673.x PG 14 WC Plant Sciences SC Plant Sciences GA 405JH UT WOS:000167155900003 ER PT J AU Penfold, LM Harnal, V Lynch, W Bird, D Derrickson, SR Wildt, DE AF Penfold, LM Harnal, V Lynch, W Bird, D Derrickson, SR Wildt, DE TI Characterization of Northern pintail (Anas acuta) ejaculate and the effect of sperm preservation on fertility SO REPRODUCTION LA English DT Article ID POULTRY SEMEN EXTENDER; ARTIFICIAL-INSEMINATION; FOWL SPERMATOZOA; POPULATIONS; PLASMA; DUCKS; 5-C AB Northern pintail duck semen and sperm traits were characterized, and the fertility of cold-stored spermatozoa was investigated using artificial insemination. Excellent quality ejaculates containing high proportions of motile spermatozoa were collected from drakes within 20 s by a massage technique. Semen was collected in Beltsville poultry semen extender, pooled and cold-stored (4 degreesC) for 0, 24, 48 or 72 h. Hens were inseminated with 100 mul twice a week, and eggs were assessed for fertilization and hatch success. fertilization success was similar (P >0.05) for semen cold-stored for 0 (51.6%), 24 (51.5%), 48 (41.1%) and 72 h (22.3%; P >0.05). Similar (P >0.05) percentages of fertilized eggs hatched to live offspring (73.1, 71.4, 87.0 and 80.0%, respectively). Fresh semen was also equilibrated with 1 or 4% dimethylsulphoxide or glycerol, and cryopreserved at the following rates: (1) approximately 60 degreesC min(-1) (in liquid nitrogen [LN2] vapour) for 10 min; (2) 1 degreesC min(-1) to -20 degreesC, LN2 vapour for 10 min; and (3) 1 degreesC min(-1) to -35 degreesC, all followed by immersion in LN2. After thawing for 30 s at 37 degreesC or 20 min at 4 degreesC, sperm motility and viability were assessed. The highest numbers of motile spermatozoa were recovered after slow-fast freezing (2) and thawing at 0 degreesC (P <0.05), but survival was inadequate to allow artificial insemination. Nonetheless, cold storage provides an effective means of short-term storage with no loss of fertility in this waterfowl species. C1 Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA 22630 USA. RP Penfold, LM (reprint author), Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA 22630 USA. NR 46 TC 17 Z9 17 U1 0 U2 2 PU JOURNALS OF REPRODUCTION FERTILITY LTD PI CAMBRIDGE PA 22 NEWMARKET RD, CAMBRIDGE CB5 8DT, ENGLAND SN 1470-1626 J9 REPRODUCTION JI Reproduction PD FEB PY 2001 VL 121 IS 2 BP 267 EP 275 PG 9 WC Developmental Biology; Reproductive Biology SC Developmental Biology; Reproductive Biology GA 426BH UT WOS:000168329100010 PM 11226051 ER PT J AU Laurance, WF Didham, RK Power, ME AF Laurance, WF Didham, RK Power, ME TI Ecological boundaries - a search for synthesis SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Editorial Material C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Canterbury, Dept Zool, Christchurch, New Zealand. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM wfl@inpa.gov.br RI Didham, Raphael/B-5953-2011; Laurance, William/B-2709-2012 NR 0 TC 35 Z9 44 U1 2 U2 20 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD FEB PY 2001 VL 16 IS 2 BP 70 EP 71 DI 10.1016/S0169-5347(00)02070-X PG 2 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 428GR UT WOS:000168453800024 ER PT J AU Phillips, DF Fleischhauer, A Mair, A Walsworth, RL Lukin, MD AF Phillips, DF Fleischhauer, A Mair, A Walsworth, RL Lukin, MD TI Storage of light in atomic vapor SO PHYSICAL REVIEW LETTERS LA English DT Article ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; GROUP-VELOCITY; ENSEMBLE; GAS AB We report an experiment in which a light pulse is effectively decelerated and trapped in a vapor of Rb atoms, stored for a controlled period of time, and then released on demand. We accomplish this "storage of light" by dynamically reducing the group velocity of the light pulse to zero, so that the coherent excitation of the light is reversibly mapped into a Zeeman (spin) coherence of the Rb vapor. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Phillips, DF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 22 TC 1425 Z9 1492 U1 11 U2 89 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JAN 29 PY 2001 VL 86 IS 5 BP 783 EP 786 DI 10.1103/PhysRevLett.86.783 PG 4 WC Physics, Multidisciplinary SC Physics GA 396FN UT WOS:000166625800009 PM 11177939 ER PT J AU West, SA Murray, MG Machado, CA Griffin, AS Herre, EA AF West, SA Murray, MG Machado, CA Griffin, AS Herre, EA TI Testing Hamilton's rule with competition between relatives SO NATURE LA English DT Article ID VISCOUS POPULATIONS; INCLUSIVE FITNESS; KIN SELECTION; FIG WASPS; ENVIRONMENT; EVOLUTION; CONFLICT; ALTRUISM AB Hamilton's(1,2) theory of kin selection suggests that individuals should show less aggression, and more altruism, towards closer kin. Recent theoretical work has, however, suggested that competition between relatives can counteract kin selection for altruism(3-11). Unfortunately, factors that tend to increase the average relatedness of interacting individuals-such as limited dispersal-also tend to increase the amount of competition between relatives. Therefore, in most natural systems, the conflicting influences of increased competition and increased relatedness are confounded, limiting attempts to test theory(4,8-10). Fig wasp taxa exhibit varying levels of aggression among non-dispersing males that show a range of average relatedness levels. Thus, across species, the effects of relatedness and competition between relatives can be separated. Here we report that-contrary to Hamilton's original prediction(1,2,12) but in agreement with recent theory(5-11) - the level of fighting between males shows no correlation with the estimated relatedness of interacting males, but is negatively correlated with future mating opportunities. C1 Univ Edinburgh, Inst Cell Anim & Populat Biol, Edinburgh EH9 3JT, Midlothian, Scotland. Rutgers State Univ, Dept Genet, Piscataway, NJ 08854 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP West, SA (reprint author), Univ Edinburgh, Inst Cell Anim & Populat Biol, W Mains Rd, Edinburgh EH9 3JT, Midlothian, Scotland. RI Machado, Carlos/B-8855-2009; Griffin, Ashleigh/C-6244-2014; West, Stuart/M-3608-2014 OI Machado, Carlos/0000-0003-1546-7415; Griffin, Ashleigh/0000-0001-7674-9825; West, Stuart/0000-0003-2152-3153 NR 30 TC 173 Z9 182 U1 9 U2 62 PU MACMILLAN PUBLISHERS LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 25 PY 2001 VL 409 IS 6819 BP 510 EP 513 DI 10.1038/35054057 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 395FW UT WOS:000166570500047 PM 11206546 ER PT J AU Vardi, A Anglin, JR AF Vardi, A Anglin, JR TI Bose-Einstein condensates beyond mean field theory: Quantum backreaction as decoherence SO PHYSICAL REVIEW LETTERS LA English DT Article ID OSCILLATIONS; DYNAMICS AB We propose an experiment to measure the slow log(N) convergence to mean field theory (MFT) around a dynamical instability. Using a density matrix formalism instead of the standard macroscopic wave function approach, we derive equations of motion which go beyond MFT and provide accurate predictions for the quantum break time. The lending quantum corrections appear as decoherence of the reduced single-particle quantum state. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Vardi, A (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. RI Vardi, Amichay/D-8189-2011 OI Vardi, Amichay/0000-0002-8992-2129 NR 19 TC 153 Z9 155 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JAN 22 PY 2001 VL 86 IS 4 BP 568 EP 571 DI 10.1103/PhysRevLett.86.568 PG 4 WC Physics, Multidisciplinary SC Physics GA 394TT UT WOS:000166539900003 PM 11177883 ER PT J AU Kochanek, CS Keeton, CR McLeod, BA AF Kochanek, CS Keeton, CR McLeod, BA TI The importance of Einstein rings SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; distance scale; gravitational lensing ID GRAVITATIONAL LENS; TIME-DELAY; PG-1115+080; Q0957+561; REDSHIFTS; GALAXIES AB We develop a theory of Einstein rings and demonstrate it using the infrared Einstein ring images of the quasar host galaxies observed in PG 1115+080, B1608+656, and B1938+666. The shape of an Einstein ring accurately and independently determines the shape of the lens potential and the shape of the lensed host galaxy. We find that the host galaxies of PG 1115+080, B1608+656, and B1938+666 have axis ratios of 0.58 +/- 0.02, 0.69 +/- 0.02, and 0.62 +/- 0.14, respectively, including the uncertainties in the lens models. The Einstein rings break the degeneracies in the mass distributions or Hubble constants inferred from observations of gravitational lenses. In particular, the Einstein ring in PG 1115+080 rules out the centrally concentrated mass distributions that lead to a high Hubble constant (H-o >60 km s(-1) Mpc(-1)) given the measured time delays. Deep, detailed observations of Einstein rings will be revolutionary for constraining mass models and determining the Hubble constant from time-delay measurements. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Kochanek, CS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 44 TC 88 Z9 88 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2001 VL 547 IS 1 BP 50 EP 59 DI 10.1086/318350 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 395RN UT WOS:000166595200005 ER PT J AU Hatziminaoglou, E Siemiginowska, A Elvis, M AF Hatziminaoglou, E Siemiginowska, A Elvis, M TI Accretion disk instabilities, cold dark matter models, and their role in quasar evolution SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; cosmology : theory; quasars : general ID ACTIVE GALACTIC NUCLEI; FRANCE REDSHIFT SURVEY; RADIO-LOUD QUASARS; LUMINOSITY FUNCTION; HOST GALAXIES; MULTICOLOR SURVEY; POWER SPECTRUM; BLACK-HOLES; CLOSE PAIRS; QSOS AB We have developed a consistent analytical model to describe the observed evolution of the quasar luminosity function. Our model combines black hole mass distributions based on the Press-Schechter theory of structure formation in the universe with quasar luminosity functions resulting from a physics-based emission model that takes into account the time-dependent phenomena occurring in the accretion disks. Quasar evolution and cold dark matter (CDM) models are mutually constraining; therefore, our model gives an estimation of the exponent, n, of the power spectrum, P(k), which is found to be -1.8 less than or equal to n less than or equal to -1.6. We were able to reject a generally assumed hypothesis of a constant ratio between dark matter halo and black hole mass, since the observed data could not be fitted under this assumption. We found that the relation between the dark matter halos and black hole masses is better described by This model provides a reasonable fit to the observed quasar luminosity function at M-BH = M-DMH(0.668). redshifts higher than similar to2.0. We suggest that the disagreement at lower redshift is due to mergers. Based on the agreement at high redshift, we estimated the merger rate at lower redshift, and argue that this rate should depend on the redshift, as (1+z)(3). C1 Lab Astrophys Toulouse, Toulouse, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hatziminaoglou, E (reprint author), Lab Astrophys Toulouse, Toulouse, France. NR 76 TC 26 Z9 26 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2001 VL 547 IS 1 BP 90 EP 98 DI 10.1086/318325 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 395RN UT WOS:000166595200009 ER PT J AU Lentz, EJ Baron, E Lundqvist, P Branch, D Hauschildt, PH Fransson, C Garnavich, P Bastian, N Filippenko, AV Kirshner, RP Challis, PM Jha, S Leibundgut, B McCray, R Michael, E Panagia, N Phillips, MM Pun, CSJ Schmidt, B Sonneborn, G Suntzeff, NB Wang, L Wheeler, JC AF Lentz, EJ Baron, E Lundqvist, P Branch, D Hauschildt, PH Fransson, C Garnavich, P Bastian, N Filippenko, AV Kirshner, RP Challis, PM Jha, S Leibundgut, B McCray, R Michael, E Panagia, N Phillips, MM Pun, CSJ Schmidt, B Sonneborn, G Suntzeff, NB Wang, L Wheeler, JC TI Analysis of type IInSN1998S: Effects of circumstellar interaction on observed spectra SO ASTROPHYSICAL JOURNAL LA English DT Article DE radiative transfer; supernovae : individual (SN 1998S) ID SUPERNOVAE AB We present spectral analysis of early observations of the Type IIn supernova 1998S using the general non-local thermodynamic equilibrium atmosphere code PHOENIX. We model both the underlying supernova spectrum and the overlying circumstellar interaction region and produce spectra in good agreement with observations. The early spectra are well fitted by lines produced primarily in the circumstellar region itself, and later spectra are due primarily to the supernova ejecta. Intermediate spectra are affected by both regions. A mass-loss rate of order (M) over dot similar to 0.0001-0.001 M. yr(-1) is inferred for a wind speed of 100-1000 km s(-1). We discuss how future self-consistent models will better clarify the underlying progenitor structure. C1 Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. Stockholm Observ, SE-13336 Saltsjobaden, Sweden. Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. Univ Notre Dame, Dept Phys, Notre Dame, IN USA. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, D-85748 Garching, Germany. Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Carnegie Inst Washington, Las Campanas Observ, La Serena, Chile. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. Australian Natl Univ, Mt Stromlo Observ, Weston Creek PO, ACT 2611, Australia. Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Lentz, EJ (reprint author), Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. RI Baron, Edward/A-9041-2009; Sonneborn, George/D-5255-2012; Lentz, Eric/M-7173-2015; OI Baron, Edward/0000-0001-5393-1608; Lentz, Eric/0000-0002-5231-0532; Schmidt, Brian/0000-0001-6589-1287 NR 20 TC 26 Z9 26 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2001 VL 547 IS 1 BP 406 EP 411 DI 10.1086/318363 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 395RN UT WOS:000166595200042 ER PT J AU Narita, T Grindlay, JE Barret, D AF Narita, T Grindlay, JE Barret, D TI ASCA observations of GX 354-0 and KS 1731-260 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; stars : individual (GX 354-0, KS 17310260); stars : neutron; X-rays : stars ID X-RAY BINARIES; BURSTER KS-1731-260; ENERGY-SPECTRA; LINE EMISSION; MASS; DISCOVERY; ROSAT; COMPTONIZATION; ACCRETION AB We report on ASCA observations of the low-mass X-ray binaries GX 354-0 and KS 1731-260. The spectrum of GX 354-0 is best described as a power law or a Comptonized spectrum with tau similar to 5 and kT similar to 8 keV and a residual at similar to6.5 keV. The residual may be a disk reflection or a Compton-broadened Gaussian line from the hot inner advection-dominated accretion flow-like coronal region. The absorption column density to the source is 2.9 x 10(22) cm(-2). No soft thermal component was detected. The spectrum from KS 1731-260 is softer, and it is best fit with a two-component model with a column density of 1.1 x 10(22) cm(-2). The likely interpretation is emission from a Comptonizing cloud with an optical depth tau > 12 and either a neutron star or a disk blackbody emission. We discuss the likely location of the Comptonizing cloud for both sources within the context of several proposed emission models. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ctr Etud Spatiale Rayonnements, Toulouse 04, France. RP Narita, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 43 TC 20 Z9 20 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2001 VL 547 IS 1 BP 420 EP 427 DI 10.1086/318326 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 395RN UT WOS:000166595200044 ER PT J AU Drake, JJ Kashyap, V AF Drake, JJ Kashyap, V TI The coronal metallicity of the intermediate activity dwarf zeta Bootis A SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : abundances; stars : activity; stars : coronae; stars : individual (zeta Bootis A) ID X-RAY SPECTROSCOPY; BEPPOSAX OBSERVATION; ROSAT OBSERVATIONS; EUVE OBSERVATIONS; METAL ABUNDANCES; AB DORADUS; COOL STARS; II-PEGASI; BETA-CETI; SOLAR AB Extreme Ultraviolet Explorer (EUVE) spectra from a 270 ks observation of the intermediate activity star xi Boo A (G8 V) have been analyzed in order to determine the metallicity of its coronal plasma. This analysis was based on a new method that used both the EUVE spectroscopic and photometric (Deep Survey) data, together with theoretical model spectra. By comparison of observed and synthetic spectra computed using the CHIANTI database, we estimated that about 20% of the observed line flux is not accounted for in the theoretical model. Allowing for the "missing lines" in our analysis, we obtain a coronal metallicity for xi Boo A of [M/H] = 0.1(-0.15)(+0.2) relative to the solar photosphere. This is slightly higher than the photospheric metallicity of [M/H] = -0.15 +/- 0.05 and lends support to the results of our earlier analysis of the same spectral data that indicated that coronal abundances of elements with low first ionization potentials (FIPs) are systematically higher than those of elements with high FIPs. These results, coupled with other evidence, imply that stars of intermediate activity level-stars more active than the Sun but significantly less active than the most active single and binary stars-do not suffer from any depletion of metals in their coronae as some coronal metallicities estimated for more active stars have appeared to suggest. The observation of a solar-like FIP effect on xi Boo A adds support to the notion that stars of intermediate activity level have coronae characterized by a high surface coverage of bright solar-like active regions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Drake, JJ (reprint author), Harvard Smithsonian Ctr Astrophys, MS-3,60 Garden St, Cambridge, MA 02138 USA. NR 70 TC 11 Z9 11 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2001 VL 547 IS 1 BP 428 EP 436 DI 10.1086/318324 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 395RN UT WOS:000166595200045 ER PT J AU Apponi, AJ Sanz, ME Gottlieb, CA McCarthy, MC Thaddeus, P AF Apponi, AJ Sanz, ME Gottlieb, CA McCarthy, MC Thaddeus, P TI The cyclic C5H radical SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : molecules; line : identification; molecular data; molecular processes; radio lines : ISM ID LABORATORY DETECTION; C3H2; CYCLOPROPENYLIDENE AB Cyclic C5H, the free radical formed by substituting an ethynyl group CCH for the hydrogen atom in the astronomical molecule c-C3H, has been detected in the laboratory in a supersonic molecular beam by Fourier transform microwave spectroscopy. Enough lines in the rotational spectrum have been measured to allow a deep search for this radical with radio telescopes. Contrary to theoretical prediction, c-C5H is apparently unsymmetrical, plausibly the result of pseudo-Jahn-Teller deformation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Univ Valladolid, Dept Quim Fis, Valladolid 47004, Spain. RP Apponi, AJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Sanz, Maria Eugenia/F-7054-2013; OI McCarthy, Michael/0000-0001-9142-0008 NR 17 TC 13 Z9 13 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2001 VL 547 IS 1 BP L65 EP L68 DI 10.1086/318887 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 395RT UT WOS:000166595600016 ER PT J AU Kenyon, SJ Windhorst, RA AF Kenyon, SJ Windhorst, RA TI The Kuiper Belt and Olbers's paradox SO ASTROPHYSICAL JOURNAL LA English DT Article DE Kuiper Belt; solar system : formation ID OUTER SOLAR-SYSTEM; COMPACT RADIO GALAXY; OBJECTS; CONSTRAINTS; FRAGMENTATION; ACCRETION; MODELS; COMETS AB We investigate the constraints that Olbers's paradox, applied to the zodiacal background as measured from space, sets on outer solar system objects. If extended to very faint limits, mag, the steep optical R similar to 40-50 number counts of Kuiper Belt objects (KBOs) at R less than or similar to 26 imply an infinitely bright night sky. Small KBOs with radii of r similar to 1 mum to r similar to 1 km must have a size distribution n(r) proportional to r(-a), with a similar to 3.4 or smaller to satisfy the known limits on the sky-surface brightness at optical and far-infrared wavelengths. Improved limits on the measured KBO surface brightness can yield direct estimates of the albedo, temperature, and size distribution for small KBOs in the outer solar system. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 35 TC 14 Z9 14 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2001 VL 547 IS 1 BP L69 EP L73 DI 10.1086/318885 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 395RT UT WOS:000166595600017 ER PT J AU Matsumoto, H Tsuru, TG Koyama, K Awaki, H Canizares, CR Kawai, N Matsushita, S Kawabe, R AF Matsumoto, H Tsuru, TG Koyama, K Awaki, H Canizares, CR Kawai, N Matsushita, S Kawabe, R TI Discovery of a luminous, variable, off-center source in the nucleus of M82 with the Chandra High-Resolution Camera SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (M82); galaxies : starburst; X rays : galaxies ID GALAXY M82; H-I; RAY; RADIO; AXAF; HRC AB We present results from observations of the most famous starburst galaxy M82 with the High-Resolution Camera on board the Chandra X-Ray Observatory. We found nine sources in the central 1' x 1' region, but no source was detected at the galactic center. Comparing the observations on 1999 October 28 and on 2000 January 20, we found that four of the nine sources showed significant time variability. In particular, CXOM82 J095550.2+694047, which is 9 " away from the galactic center, showed extremely large time variability. We conclude that this source is the origin of the hard X-ray time variability of M82 detected with ASCA. Assuming a spectral shape obtained by the ASCA observation, its luminosity in the 0.5-10 keV band changed from 1.2 x 10(40) ergs s(-1) on 1999 October 28 to8.7 x 10(40) ergs s(-1) on 2000 January 20. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Kyoto Univ, Fac Sci, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. Japan Sci & Technol Corp, CREST, Kawaguchi, Saitama 3320012, Japan. Ehime Univ, Fac Sci, Matsuyama, Ehime 7908577, Japan. RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan. Harvard Smithsonian Ctr Astrophys, Smithsonian Submillimeter Array, Hilo, HI 96720 USA. Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. RP Matsumoto, H (reprint author), MIT, Ctr Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. NR 25 TC 175 Z9 176 U1 2 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2001 VL 547 IS 1 BP L25 EP L28 DI 10.1086/318878 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 395RT UT WOS:000166595600006 ER PT J AU Zhao, JH Bower, GC Goss, WM AF Zhao, JH Bower, GC Goss, WM TI Radio variability of Sagittarius A* - A 106 day cycle SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : active; Galaxy : center; radio continuum : galaxies ID PROPER-MOTION; GALAXY AB We report the presence of a 106 day cycle in the radio variability of Sagittarius A* based on an analysis of data observed with the Very Large Array over the past 20 years. The pulsed signal is most clearly seen at 1.3 cm with a ratio of cycle frequency to frequency width f/Deltaf = 2.2 +/- 0.3. The periodic signal is also clearly observed at 2 cm. At 3.6 cm the detection of a periodic signal is marginal. No significant periodicity is detected at both 6 and 20 cm. Since the sampling function is irregular, we performed a number of tests to ensure that the observed periodicity is not the result of noise. Similar results were found for a maximum entropy method and a periodogram with a CLEAN method. The probability of false detection for several different noise distributions is less than 5% based on Monte Carlo tests. The radio properties of the pulsed component at 1.3 cm are a spectral index alpha similar to 1.0 +/- 0.1 (for S proportional to nu (alpha)), an amplitude DeltaS = 0.42 +/- 0.04 Jy, and a characteristic timescale Deltat(FWHM) approximate to 25 +/- 5 days. The lack of a VLBI detection of a secondary component suggests that the variability occurs within Sgr A* on a scale of similar to5 AU, suggesting an instability of the accretion disk. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, New Mexico Array Operat Ctr, Socorro, NM 87801 USA. RP Zhao, JH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. NR 22 TC 71 Z9 72 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2001 VL 547 IS 1 BP L29 EP L32 DI 10.1086/318877 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 395RT UT WOS:000166595600007 ER PT J AU Smith, DA Ralls, K Davenport, B Adams, B Maldonado, JE AF Smith, DA Ralls, K Davenport, B Adams, B Maldonado, JE TI Canine assistants for conservationists SO SCIENCE LA English DT Letter C1 Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. Univ Washington, Seattle, WA 98195 USA. Dept Correct Canine Program, Steilacoom, WA 98388 USA. RP Ralls, K (reprint author), Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. NR 9 TC 33 Z9 35 U1 2 U2 13 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 19 PY 2001 VL 291 IS 5503 BP 435 EP 435 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 393UF UT WOS:000166487500015 PM 11228135 ER PT J AU Towe, KM AF Towe, KM TI On the origins of photosynthesis SO SCIENCE LA English DT Letter ID OXYGEN; LIFE C1 Smithsonian Inst, Tennille, GA 31089 USA. RP Towe, KM (reprint author), Smithsonian Inst, 230 W Adams St, Tennille, GA 31089 USA. NR 8 TC 7 Z9 7 U1 1 U2 10 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 19 PY 2001 VL 291 IS 5503 BP 436 EP 437 DI 10.1126/science.291.5503.436 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 393UF UT WOS:000166487500020 PM 11228138 ER PT J AU Laurance, WF Cochrane, MA Bergen, S Fearnside, PM Delamonica, P Barber, C D'Angelo, S Fernandes, T AF Laurance, WF Cochrane, MA Bergen, S Fearnside, PM Delamonica, P Barber, C D'Angelo, S Fernandes, T TI Environment - The future of the Brazilian Amazon SO SCIENCE LA English DT Editorial Material ID FORESTS; RESPONSES C1 Smithsonian Trop Res Inst, Balboa, Panama. Natl Inst Amazonian Res, BDFFP, BR-69011970 Manaus, Amazonas, Brazil. Michigan State Univ, BSRSI, E Lansing, MI 48823 USA. Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA. INPA, Dept Ecol, BR-69011970 Manaus, Amazonas, Brazil. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. RI Laurance, William/B-2709-2012; Fearnside, Philip/D-6559-2011 OI Fearnside, Philip/0000-0003-3672-9082 NR 12 TC 416 Z9 448 U1 11 U2 86 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 19 PY 2001 VL 291 IS 5503 BP 438 EP 439 DI 10.1126/science.291.5503.438 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 393UF UT WOS:000166487500023 PM 11228139 ER PT J AU Clutton-Brock, TH Brotherton, PNM Russell, AF O'Riain, MJ Gaynor, D Kansky, R Griffin, A Manser, M Sharpe, L McIlrath, GM Small, T Moss, A Monfort, S AF Clutton-Brock, TH Brotherton, PNM Russell, AF O'Riain, MJ Gaynor, D Kansky, R Griffin, A Manser, M Sharpe, L McIlrath, GM Small, T Moss, A Monfort, S TI Cooperation, control, and concession in meerkat groups SO SCIENCE LA English DT Article ID SURICATA-SURICATTA; ANIMAL SOCIETIES AB "Limited control" models of reproductive skew in cooperative societies suggest that the frequency of breeding by subordinates is determined by the outcome of power struggles with dominants. In contrast, "optimal skew" models suggest that dominants have full control of subordinate reproduction and allow subordinates to breed only when this serves to retain subordinates' assistance with rearing dominants' own Litters. The results of our 7-year field study of cooperative meerkats, Suricata suricatta, support the predictions of Limited control models and provide no indication that dominant females grant reproductive concessions to subordinates to retain their assistance with future breeding attempts. C1 Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. Univ Pretoria, Mammal Res Inst, ZA-0002 Pretoria, South Africa. Univ Edinburgh, Inst Cell Anim & Populat Biol, Edinburgh EH9 3JT, Midlothian, Scotland. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Clutton-Brock, TH (reprint author), Univ Cambridge, Dept Zool, Downing St, Cambridge CB2 3EJ, England. RI Griffin, Ashleigh/C-6244-2014 OI Griffin, Ashleigh/0000-0001-7674-9825 NR 15 TC 185 Z9 187 U1 17 U2 106 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 19 PY 2001 VL 291 IS 5503 BP 478 EP 481 DI 10.1126/science.291.5503.478 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 393UF UT WOS:000166487500039 PM 11161200 ER PT J AU Erbacher, J Huber, BT Norris, RD Markey, M AF Erbacher, J Huber, BT Norris, RD Markey, M TI Increased thermohaline stratification as a possible cause for an ocean anoxic event in the Cretaceous period SO NATURE LA English DT Article ID NORTH-ATLANTIC; ALPINE TETHYS; STRATIGRAPHY; EPISODES; SEA AB Ocean anoxic events were periods of high carbon burial that led to drawdown of atmospheric carbon dioxide, lowering of bottom-water oxygen concentrations and, in many cases, significant biological extinction(1-5). Most ocean anoxic events are thought to be caused by high productivity and export of carbon from surface waters which is then preserved in organic-rich sediments, known as black shales. But the factors that triggered some of these events remain uncertain. Here we present stable isotope data from a mid-Cretaceous ocean anoxic event that occurred 112 Myr ago, and that point to increased thermohaline stratification as the probable cause. Ocean anoxic event 1b is associated with an increase in surface-water temperatures and runoff that led to decreased bottom-water formation and elevated carbon burial in the restricted basins of the western Tethys and North Atlantic. This event is in many ways similar to that which led to the more recent Plio-Pleistocene Mediterranean sapropels, but the greater geographical extent and longer duration (similar to 46 kyr) of ocean anoxic event 1b suggest that processes leading to such ocean anoxic events in the North Atlantic and western Tethys were able to act over a much larger region, and sequester far more carbon, than any of the Quaternary sapropels. C1 Bundesanstalt Geowissensch & Rohstoffe, Referat Meeresgeol, D-30655 Hannover, Germany. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. RP Erbacher, J (reprint author), Bundesanstalt Geowissensch & Rohstoffe, Referat Meeresgeol, Stilleweg 2, D-30655 Hannover, Germany. EM erbacher@bgr.de NR 30 TC 148 Z9 159 U1 3 U2 30 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 18 PY 2001 VL 409 IS 6818 BP 325 EP 327 DI 10.1038/35053041 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 392VY UT WOS:000166434300042 PM 11201737 ER PT J AU Fracalossi, DM Allen, ME Yuyama, LK Oftedal, OT AF Fracalossi, DM Allen, ME Yuyama, LK Oftedal, OT TI Ascorbic acid biosynthesis in Amazonian fishes SO AQUACULTURE LA English DT Article DE ascorbic acid biosynthesis; Amazonian fishes; L-gulonolactone oxidase ID GULONOLACTONE OXIDASE ACTIVITY; CHANNEL CATFISH; VITAMIN-C; ICTALURUS-PUNCTATUS; AQUATIC ANIMALS; REQUIREMENT; DEFICIENCY; TELEOSTS; ABILITY; SCURVY AB The incapacity to synthesize ascorbic acid (AA) is due to the lack of activity of L-gulonolactone oxidase (GLO), which catalyzes the last step of AA biosynthesis. It was postulated that vertebrates unable to synthesize AA had sufficient amounts of this nutrient in their diet and consequently did not need to preserve synthetic capability. In the present study, we analyzed the GLO activity in kidney and liver of 13 fish species, including 11 teleosts, namely: freshwater stingray, Potamotrygon sp.; South American lungfish, Lepidosiren paradoxa; "sardinhao," Pelona sp.; arowana, Osteoglossum bicirrhosum; arapaima, Arapaima gigas; "piranha caju," Pygocentrus nattereri; "piranha mucura," Serrasalmus elongatus; "aracu," Schizodon fasciatus; "tambaqui," Colossoma macropomum; "acari-pedra," Hypostomus sp., "sarapo," Steatogenys elegans; electric eel, Electrophorus electricus; and the peacock bass, Cichla sp. Four representatives of the Characiformes order with distinct feeding habits were included in this study to evaluate the influence of feeding habit on GLO activity. Only two species of non-teleost fishes, the freshwater stingray (Miliobatiformes) and the South American lungfish (Lepidosireniformes), showed CLO activity in their kidneys, corroborating the hypothesis that teleosts are unable to synthesize AA. Additionally, as expected, we observed that the phylogenetic position is more important than feeding habit as a determinant of the biosynthetic ability since none of the Characiformes species analyzed synthesize AA, independent of their distinct feeding habits. Female freshwater stingrays had a significantly higher GLO activity than males (P < 0.05), but there was no difference in the biosynthetic capability regarding the portion of the kidney analyzed (P > 0.05), as previously reported in white sturgeon. This is the first report of the AA biosynthetic ability in South American lungfish and freshwater Elasmobranchs. (C) 2001 Elsevier Science B.V. All rights reserved. C1 Univ Fed Santa Catarina, Ctr Ciencias Agr, Dept Aquicultura, BR-88040900 Florianopolis, SC, Brazil. Smithsonian Inst, Natl Zool Pk, Dept Nutr Resources, Washington, DC 20008 USA. Inst Nacl Pesquisas Amazonia, Coordenacao Pesquisas Ciencias Saude, BR-69083000 Manaus, Amazonas, Brazil. Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. RP Fracalossi, DM (reprint author), Univ Fed Santa Catarina, Ctr Ciencias Agr, Dept Aquicultura, Rodovia SC 404,Km 3,CP 476, BR-88040900 Florianopolis, SC, Brazil. NR 43 TC 43 Z9 64 U1 7 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0044-8486 J9 AQUACULTURE JI Aquaculture PD JAN 15 PY 2001 VL 192 IS 2-4 BP 321 EP 332 DI 10.1016/S0044-8486(00)00455-5 PG 12 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 397UT UT WOS:000166716300019 ER PT J AU Bush, M Grobler, DG Raath, JP Phillips, LG Stamper, MA Lance, WR AF Bush, M Grobler, DG Raath, JP Phillips, LG Stamper, MA Lance, WR TI Use of medetomidine and ketamine for immobilization of free-ranging giraffes SO JOURNAL OF THE AMERICAN VETERINARY MEDICAL ASSOCIATION LA English DT Article ID CAMELOPARDALIS; XYLAZINE AB Objective-To develop a dosage correlated with shoulder height (SH) in centimeters for effective immobilization of free-ranging giraffes, using a combination of medetomidine (MED) and ketamine (KET) and reversal with atipamezole (ATP). Design-Prospective study. Animals-23 free-ranging giraffes. Procedure-The drug combination (MED and KET) was administered by use of a projectile dart. Quality of induction, quality of immobilization, and lime to recovery following injection of ATP were evaluated. Physiologic variables measured during immobilization included Pao(2), Paco(2), oxygen saturation, end-tidal CO2,`blood pH, indirect arterial blood pressure, heart and respiratory rates, and rectal temperature. Results-Sixteen giraffes became recumbent with a dosage (mean +/- SD) of 143 +/- 29 mug of MED and 2.7 +/- 0.6 mg of KET/cm of SH. Initially, giraffes were atactic and progressed to lateral recumbency. Three giraffes required casting with ropes for data collection, with dosages of 166 +/- 5 mug of MED and 3.2 +/- 0.6 mg of KET/cm of SH. Four giraffes required administration of etorphine (n = 2) or were cast with ropes (2) for capture but remained dangerous to personnel once recumbent, precluding data collection. In giraffes successfully immobilized, physiologic monitoring revealed hypoxia and increased respiratory rates. Values for Paco(2), end-tidal CO2, and heart rate remained within reference ranges. All giraffes were hypertensive and had a slight increase in rectal temperature. Atipamezole was administered at 340 +/- 20 mug/cm of SH, resulting in rapid and smooth recoveries. Conclusions and Clinical Relevance-Medetomidine and KET was an effective immobilizing combination for free-ranging giraffes; however, at the dosages used, it does not induce adequate analgesia for major manipulative procedures. Quality of induction and immobilization were enhanced if the giraffe was calm. Reversal was rapid and complete following injection of ATP. C1 Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA 22630 USA. S African Natl Pk Kruger Natl Pk, ZA-1350 Skukuza, South Africa. Univ Calif Davis, Sch Vet Med, Dept Med & Epidemiol, Davis, CA 95616 USA. N Carolina State Univ, Coll Vet Med, Dept Compan Anim & Special Species Med, Raleigh, NC 27606 USA. Wildlife Pharmaceut Inc, Ft Collins, CO 80524 USA. RP Bush, M (reprint author), Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, 1500 Remount Rd, Front Royal, VA 22630 USA. NR 16 TC 13 Z9 14 U1 1 U2 9 PU AMER VETERINARY MEDICAL ASSOC PI SCHAUMBURG PA 1931 N MEACHAM RD SUITE 100, SCHAUMBURG, IL 60173-4360 USA SN 0003-1488 J9 J AM VET MED ASSOC JI J. Am. Vet. Med. Assoc. PD JAN 15 PY 2001 VL 218 IS 2 BP 245 EP 249 DI 10.2460/javma.2001.218.245 PG 5 WC Veterinary Sciences SC Veterinary Sciences GA 392GK UT WOS:000166403200039 PM 11195833 ER PT J AU Simkin, T Siebert, L Blong, R AF Simkin, T Siebert, L Blong, R TI Policy forum: Disasters - Volcano fatalities - Lessons from the historical record SO SCIENCE LA English DT Editorial Material C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. Macquarie Univ, Natl Hazards Res Ctr, N Ryde, NSW 2109, Australia. RP Simkin, T (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 4 TC 21 Z9 21 U1 0 U2 9 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 12 PY 2001 VL 291 IS 5502 BP 255 EP 255 DI 10.1126/science.291.5502.255 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 391JM UT WOS:000166352900028 PM 11253213 ER PT J AU Alves, JF Lada, CJ Lada, EA AF Alves, JF Lada, CJ Lada, EA TI Internal structure of a cold dark molecular cloud inferred from the extinction of background starlight SO NATURE LA English DT Article ID STAR-FORMATION; DUST EXTINCTION; BOK GLOBULES; IC 5146; INSTABILITY; CORES; L977; GAS AB Stars and planets form within dark molecular clouds, but little is understood about the internal structure of these clouds, and consequently about the initial conditions that give rise to star and planet formation. The clouds are primarily composed of molecular hydrogen, which is virtually inaccessible to direct observation. But the clouds also contain dust, which is well mixed with the gas and which has well understood effects on the transmission of light. Here we use sensitive near-infrared measurements of the light from background stars as it is absorbed and scattered by trace amounts of dust to probe the internal structure of the dark cloud Barnard 68 with unprecedented detail. We rnd the cloud's density structure to be very well described by the equations for a pressure-confined, self-gravitating isothermal sphere that is critically stable according to the Bonnor-Ebert criteria(1,2). As a result we can precisely specify the physical conditions inside a dark cloud on the verge of collapse to form a star. C1 European So Observ, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florida, Dept Astron, Gainesville, FL 32608 USA. RP Alves, JF (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM jalves@eso.org NR 30 TC 301 Z9 301 U1 0 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 11 PY 2001 VL 409 IS 6817 BP 159 EP 161 DI 10.1038/35051509 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 390UV UT WOS:000166316200034 PM 11196632 ER PT J AU Tonry, JL Dressler, A Blakeslee, JP Ajhar, EA Fletcher, AB Luppino, GA Metzger, MR Moore, CB AF Tonry, JL Dressler, A Blakeslee, JP Ajhar, EA Fletcher, AB Luppino, GA Metzger, MR Moore, CB TI The SBF survey of galaxy distances. IV. SBF magnitudes, colors, and distances SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; galaxies : clusters : individual (Virgo, Centaurus) galaxies : distances and redshifts; large-scale structure of universe ID SURFACE-BRIGHTNESS FLUCTUATIONS; HUBBLE-SPACE-TELESCOPE; SAMPLE SELECTION; STELLAR POPULATIONS; CONSTANT; CALIBRATION AB We report data for I-band surface brightness fluctuation (SBF) magnitudes, (V - I) colors, and distance moduli for 300 galaxies. The survey contains E, S0, and early-type spiral galaxies in the proportions of 49: 42: 9 and is essentially complete for E galaxies to Hubble velocities of 2000 km s(-1), with a substantial sampling of E galaxies out to 4000 km s(-1). The median error in distance modulus is 0.22 mag. We also present two new results from the survey. (1) We compare the mean peculiar flow velocity (bulk flow) implied by our distances with predictions of typical cold dark matter transfer functions as a function of scale, and we find very good agreement with cold, dark matter cosmologies if the transfer function scale parameter Gamma and the power spectrum normalization sigma (8) are related by sigma (8) Gamma (-0.25) approximate to 2 +/- 0.5. Derived directly from velocities, this result is independent of the distribution of galaxies or models for biasing. This modest bulk flow contradicts reports of large-scale, large-amplitude flows in the similar to 200 Mpc diameter volume surrounding our survey volume. (2) We present a distance-independent measure of absolute galaxy luminosity, (N) over bar and show how it correlates with galaxy properties such as color and velocity dispersion, demonstrating its utility for measuring galaxy distances through large and unknown extinction. C1 Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Carnegie Observ, Pasadena, CA 91101 USA. Univ Durham, Dept Phys, Durham DH1 3LE, England. Kitt Peak Natl Observ, Natl Opt Astron Observ, Tucson, AZ 85726 USA. MIT, Haystack Observ, Westford, MA 01886 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. RP Tonry, JL (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. NR 34 TC 877 Z9 880 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2001 VL 546 IS 2 BP 681 EP 693 DI 10.1086/318301 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393GH UT WOS:000166460500007 ER PT J AU Munoz, JA Falco, EE Kochanek, CS Lehar, J McLeod, BA McNamara, BR Vikhlinin, AA Impey, CD Rix, HW Keeton, CR Peng, CY Mullis, CR AF Munoz, JA Falco, EE Kochanek, CS Lehar, J McLeod, BA McNamara, BR Vikhlinin, AA Impey, CD Rix, HW Keeton, CR Peng, CY Mullis, CR TI Multifrequency analysis of the new wide-separation gravitational lens candidate RX J0921+4529 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; quasars : individual (RX J0921+4529) ID COSMOLOGICAL MODELS; QUASAR; DARK; Q1634+267A,B; LIMITS AB We report the discovery of a new two-image gravitational lens candidate. The system RX J0921+4529 contains two z(s) = 1.66 quasars separated by 6."93 with an H-band magnitude difference of Deltam=1.39. The HST NIC2 H-band images reveal an H=18.2 spiral galaxy between the quasar images, which is probably a member of a z(l) = 0.32 X-ray cluster centered on the field. We detect an extended source near the fainter quasar image but not in the brighter image. If this extended source is the host galaxy of the fainter quasar, then the system is a binary quasar rather than a gravitational lens. VLA observations at 3.6 cm reveal emission from the lens galaxy at the flux level of 1 mJy and a marginal detection of the brighter quasar. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Inst Astrofis Canarias, E-38200 La Laguna, Tenerife, Spain. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Max Planck Inst Astrophys, D-69117 Heidelberg, Germany. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Munoz, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 22 TC 21 Z9 21 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2001 VL 546 IS 2 BP 769 EP 774 DI 10.1086/318322 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393GH UT WOS:000166460500013 ER PT J AU McLeod, KK McLeod, BA AF McLeod, KK McLeod, BA TI NICMOS observations of low-redshift quasar host galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : photometry; infrared : galaxies; quasars : general ID RADIO-QUIET QUASARS; LUMINOUS QUASARS; LOUD QUASARS; IMAGES AB We have obtained Near-Infrared Camera and Multi-Object Spectrometer images of 16 radio-quiet quasars observed as part of a project to investigate the "luminosity/host-mass limit." The limit results were presented in a paper by McLeod, Rieke, & Storrie-Lombardi. In this paper, we present the images themselves, along with one- and two-dimensional analyses of the host galaxy properties. We find that our model-independent one-dimensional technique is reliable for use on ground-based data at low redshifts; that many radio-quiet quasars live in de Vaucouleurs-law hosts, although some of the techniques used to determine host type are questionable; that complex structure is found in many of the hosts, but that there are some hosts that are very smooth and symmetric; and that the nuclei radiate at similar to2%-20% of the Eddington rate based on the assumption that all galaxies have central black holes with a constant mass fraction of 0.6%. Despite targeting hard-to-resolve hosts, we have failed to find any that imply super-Eddington accretion rates. C1 Wellesley Coll, Whitin Observ, Wellesley, MA 02481 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wellesley Coll, Whitin Observ, Wellesley, MA 02481 USA. EM kmcleod@wellesley.edu; bmcleod@cfa.harvard.edu NR 23 TC 54 Z9 54 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2001 VL 546 IS 2 BP 782 EP 794 DI 10.1086/318306 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393GH UT WOS:000166460500015 ER PT J AU Gallagher, SC Brandt, WN Laor, A Elvis, M Mathur, S Wills, BJ Iyomoto, N AF Gallagher, SC Brandt, WN Laor, A Elvis, M Mathur, S Wills, BJ Iyomoto, N TI Heavy X-ray absorption in soft X-ray-weak active galactic nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (PG 1011-040, PG 1535+547,PG 2112+059, Markarian 486) quasars : absorption lines; X-rays : galaxies ID BRIGHT QUASAR SURVEY; HUBBLE-SPACE-TELESCOPE; ROSAT OBSERVATIONS; LINE QUASARS; OPTICAL VARIABILITY; EMISSION-LINE; CONTINUUM; SAMPLE; POLARIZATION; OBJECTS AB Recent ROSAT studies have identified a significant population of active galactic nuclei (AGNs) that are notably faint in soft X-rays relative to their optical fluxes. Are these AGNs intrinsically X-ray weak or are they highly absorbed? Brandt, Laor, & Wills have systematically examined the optical and UV spectral properties of a well-defined sample of these soft X-ray-weak (SXW) AGNs drawn from the Boroson & Green sample of all the Palomar Green AGNs with z <0.5. We present ASCA observations of three of these SXW AGNs: PG 1011-040, PG 1535+547 (Mrk 486), and PG 2112+059. In general, our ASCA observations support the intrinsic absorption scenario for explaining soft X-ray weakness; both PG 1535+547 and PG 2112+059 show significant column densities (N-H 10(22)-10(23) cm(-2)) of absorbing gas. Interestingly, PG 1011-040 shows no spectral evidence for X-ray absorption. The weak X-ray emission may result from very strong absorption of a partially covered source, or this AGN may be intrinsically X-ray weak. PG 2112+059 is a broad absorption line (BAL) QSO, and we find it to have the highest X-ray flux known of this class. It shows a typical power-law X-ray continuum above 3 keV; this is the first direct evidence that BAL QSOs indeed have normal X-ray continua underlying their intrinsic absorption. Finally, marked variability between the ROSAT and ASCA observations of PG 1535+547 and PG 2112+059 suggests that the soft X-ray-weak designation may be transient, and multiepoch 0.1-10.0 keV X-ray observations are required to constrain variability of the absorber and continuum. C1 Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Inst Space & Astronaut Sci, Kanagawa 2298510, Japan. RP Gallagher, SC (reprint author), Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. RI Brandt, William/N-2844-2015 OI Brandt, William/0000-0002-0167-2453 NR 54 TC 72 Z9 73 U1 1 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2001 VL 546 IS 2 BP 795 EP 804 DI 10.1086/318294 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393GH UT WOS:000166460500016 ER PT J AU Mahdavi, A AF Mahdavi, A TI The orbital structure of dark matter halos with gas SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : general; galaxies : clusters : individual (Cl 0024+16, Abell 2199); hydrodynamics; X-rays : galaxies ID X-RAY; GALAXY CLUSTERS; COOLING FLOWS; MASS; DYNAMICS; CATALOG; SYSTEMS; MODELS AB With the success of the Chandra and XMM missions and the maturation of gravitational lensing techniques, powerful constraints on the orbital structure of cluster dark matter halos are possible. I show that the X-ray emissivity and mass of a galaxy cluster uniquely specify the anisotropy and velocity dispersion profiles of its dark matter halo. I consider hydrostatic as well as cooling flow scenarios and apply the formalism to the lensing cluster Cl 0024+16 and the cooling flow cluster Abell 2199. In both cases, the model predicts a parameter-free velocity dispersion profile that is consistent with independent optical redshift surveys of the clusters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mahdavi, A (reprint author), Harvard Smithsonian Ctr Astrophys, MS 10,60 Garden St, Cambridge, MA 02138 USA. NR 34 TC 4 Z9 4 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2001 VL 546 IS 2 BP 812 EP 824 DI 10.1086/318286 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393GH UT WOS:000166460500018 ER PT J AU Blout, BD Daw, EJ Decowski, MP Ho, PTP Rosenberg, LJ Yu, DB AF Blout, BD Daw, EJ Decowski, MP Ho, PTP Rosenberg, LJ Yu, DB TI A radio telescope search for axions SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; elementary particles; galaxies : dwarf; radio lines : general ID CP INVARIANCE; GALAXIES AB The axion is a hypothetical elementary particle and a cold dark matter candidate. It could dominate the potential wells of most astrophysical objects. Axions spontaneously decay into nearly monochromatic microwave photons. We present results from a radio telescope search for these axion decay photons of mass m(a) = 298-363 mu eV in Local Group dwarf galaxies. We report a limit on the axion-to- two-photon coupling constant g(a gamma gamma) >10 x 10(-9) GeV-1. C1 MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Nucl Sci Lab, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Blout, BD (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. RI Decowski, Patrick/A-4341-2011 NR 21 TC 11 Z9 11 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2001 VL 546 IS 2 BP 825 EP 828 DI 10.1086/318310 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393GH UT WOS:000166460500019 ER PT J AU Smith, AM Collins, NR Waller, WH Roberts, MS Smith, DA Bohlin, RC Cheng, KP Fanelli, MN Neff, SG O'Connell, RW Parise, RA Smith, EP Stecher, TP AF Smith, AM Collins, NR Waller, WH Roberts, MS Smith, DA Bohlin, RC Cheng, KP Fanelli, MN Neff, SG O'Connell, RW Parise, RA Smith, EP Stecher, TP TI Far-ultraviolet imagery of the edge-on spiral galaxy NGC 4631 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 4631); galaxies : ISM; galaxies : kinematics and dynamics; galaxies : starburst; galaxies : star clusters; ultraviolet : galaxies ID STAR-FORMATION; ENERGY-DISTRIBUTIONS; IMAGING TELESCOPE; H-I; NGC-4631; STARBURST; CATALOG; SUPERSHELLS; EXTINCTION; PHOTOMETRY AB Far-ultraviolet (FUV) imagery of the edge-on, Sc/SBd galaxy NGC 4631 reveals very strong FUV emission, resulting from active star formation, uniformly distributed along the galactic midplane. Multiband imagery, H I and H II position-velocity curves, and extinction considerations all imply that the emission is from the outer edges of the visible galaxy. The overall FUV morphology of this edge-on disk system is remarkably similar to those of the "chain galaxies" evident at high redshift, thus suggesting a similar interpretation for at least some of those distant objects. FUV, U, B, and V magnitudes, measured for 48 star-forming regions, along with corresponding H alpha and H beta measurements are used to construct diagnostic color-color diagrams. Although there are significant exceptions, most of the star-forming regions are less massive and older than 30 Doradus. Comparison with the expectations from two star formation models yields ages of 2.7 to 10 Myr for the instantaneous burst (IB) model and star formation cutoff ages of 0 to 9 Myr for the continuous star formation (CSF) model. Interpreted in terms of the IB model the photometry implies a total created mass in the 48 star-forming regions of 2.5 x 10(7) M-.. When viewed as resulting from constant star formation the photometry implies a star formation rate of 0.33 M-. yr(-1). These results are compared to those derived from FIR and radio observations. Corrections for FUV emission reprocessed by interstellar grains are estimated. A large ring, similar to3 kpc in diameter, of 14 star-forming regions is concentrically located with an expanding H I shell toward the eastern end of the galaxy. Our observations imply that the shell may have been generated primarily by supernovae arising from 5.3]10(4) OB stars in a massive star-forming region beginning about 20 Myr ago, and that the presently observed FUV bright emission is due to second generation stars. C1 NASA, Astron & Solar Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NASA, Raytheon STX Corp, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tufts Univ, Medford, MA 02155 USA. Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Calif State Univ Fullerton, Dept Phys, Fullerton, CA 92634 USA. Univ N Texas, Dept Phys, Denton, TX 76203 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. NASA, Comp Sci Corp, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Smith, AM (reprint author), NASA, Astron & Solar Phys Lab, Goddard Space Flight Ctr, Code 681, Greenbelt, MD 20771 USA. NR 53 TC 12 Z9 12 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2001 VL 546 IS 2 BP 829 EP 844 DI 10.1086/318273 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393GH UT WOS:000166460500020 ER PT J AU Cagnoni, I Fruscione, A AF Cagnoni, I Fruscione, A TI Four years of extreme ultraviolet observations of Markarian 421. I. Spectral analysis SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (Markarian 421); galaxies : active; galaxies : individual (Markarian 421); galaxies : nuclei; ultraviolet : galaxies ID X-RAY-SPECTRUM; ALL-SKY SURVEY; LACERTAE OBJECT MARKARIAN-421; SELF-COMPTON MODELS; RESONANT ABSORPTION; SOURCE CATALOG; EXPLORER; PKS-2155-304; PKS-0548-322; CALIBRATION AB We analyzed the similar to 950 ks of spectroscopic data accumulated by the Extreme Ultraviolet Explorer (EUV E) satellite between 1994 and 1997 for the BL Lacertae object Markarian 421. The EUV spectrum is well detected in the 70-110 Angstrom (112-177 eV) range and can be fitted by a power-law model plus an absorption feature in the similar to 71-75 Angstrom range. Previous studies of EUV absorption features in Mrk 421 and in the other EUV bright BL Lac object, PKS 2155-304, explain this absorption feature as a superposition of Doppler-smeared absorption lines (mainly L- and M-shell transitions of Mg and Ne) originating in high-velocity gas clouds ionized by the beamed continuum of the associated relativistic jet. We show that, for example, Fe IX L could also be a possibility consistent with the marginal detection of oxygen absorption lines in the X-ray range. However physical models are highly sensitive to the assumptions on the photoionizing continuum and the surrounding gas. C1 SISSA, I-34138 Trieste, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cagnoni, I (reprint author), SISSA, Via Beirut 4, I-34138 Trieste, Italy. NR 50 TC 1 Z9 1 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2001 VL 546 IS 2 BP 877 EP 885 DI 10.1086/318274 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393GH UT WOS:000166460500023 ER PT J AU Cagnoni, I Papadakis, IE Fruscione, A AF Cagnoni, I Papadakis, IE Fruscione, A TI Four years of extreme ultraviolet observations of Markarian 421. II. Temporal analysis SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (Markarian 421); galaxies : active; galaxies : individual (Markarian 421); galaxies : nuclei; ultraviolet : galaxies ID BL LACERTAE OBJECTS; SELF-COMPTON MODEL; X-RAY VARIABILITY; POWER SPECTRUM; FREQUENCIES AB The Extreme Ultraviolet Explorer (EUV E) satellite accumulated similar to1,000,000 s of public data between 1994 and 1997 for the BL Lacertae object Markarian 421. This is the second of two papers in which we present the results of spectral and temporal analysis of this EUV E data set. We analyze in the present paper the imaging data by means of power spectrum and structure function techniques, while the spectral analysis is presented in a companion paper. We find for Mrk 421 a power spectrum with slope -2.14 +/- 0.28 with a break at similar to3 days. This is the first time that a break in the power spectrum of a BL Lacertae object has been found. We also find evidence of nonstationarity for Mrk 421 EUV emission. C1 SISSA, I-34138 Trieste, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Crete, Dept Phys, Heraklion 71003, Crete, Greece. RP Cagnoni, I (reprint author), SISSA, Via Beirut 4, I-34138 Trieste, Italy. RI Papadakis, Iossif/C-3235-2011 NR 24 TC 6 Z9 6 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2001 VL 546 IS 2 BP 886 EP 897 DI 10.1086/318303 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393GH UT WOS:000166460500024 ER PT J AU Navascues, DBY Stauffer, JR Bouvier, J Martin, EL AF Navascues, DBY Stauffer, JR Bouvier, J Martin, EL TI From the top to the bottom of the main sequence: A complete mass function of the young open cluster M35 SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations : individual (M35) stars : luminosity function, mass function ID BROWN DWARF CANDIDATES; PRECISE DETERMINATION; MOTION ANALYSIS; CCD PHOTOMETRY; KECK SPECTRA; PLEIADES; STARS; BOUNDARY; HYADES; AGE AB We present very deep and accurate photometry of the open cluster M35. We have observed this association in the Cousins R, I filters, together with the Johnson V filter. We have covered a region of 27.5 x 27.5 square arcmin, equivalent to a fifth of the total area of the cluster. The data range from I-c = 12.5 to 23.5 mag, and the color intervals are 0.4 less than or equal to (V - I)c less than or equal to 3.0, 0.5 less than or equal to (R - I)(c) less than or equal to 2.5. Roughly, these values span from 1.6 M. down to the substellar limit, in the case of cluster members. By using the location of the stars on color-magnitude and color-color diagrams, we have selected candidate members of this cluster. We have merged our sample with previously published data and obtained a color-magnitude diagram for the complete stellar population of the cluster, covering the spectral range early B-mid M. Based on the distribution of field and cluster stars in color-magnitude and color-color diagrams, we estimate that two-thirds of these candidates are likely to be true members of M35. These stars approximately double the number of stars identified as candidate members of this cluster (similar to 2700). We provide the photometry and accurate positions of these stars. The deep photometry has allowed us to study the mass segregation within the cluster, the luminosity function, and mass function. We show that in the magnitude range 13 less than or equal to I-c less than or equal to 22 there is a reduced mass segregation, in opposition to what happens to higher mass stars, where the mass segregation is stronger. The luminosity function behaves essentially as the one characteristic of the Pleiades, presenting a peak at I-c similar to 19 mag (M-I similar to 9). Combining our photometry with previous data corresponding to more massive stars, we find that the mass function increases monotonically, when plotted in a log-log form, until it reaches similar to0.8 M. (alpha = 2.59). It remains shallower for less massive stars (alpha = 0.81 for 0.8-0.2 M.), whereas a decrease is observed for stars close to the substellar regime. These different behaviors suggest that at least three mechanisms play a role in the formation of stellar and substellar objects. The total mass of the cluster is similar to 1600 M. in the area covered by this study. C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Grenoble 1, Observ Grenoble, Astrophys Lab, F-38041 Grenoble, France. CALTECH, Pasadena, CA 91125 USA. RP Navascues, DBY (reprint author), Univ Autonoma Madrid, Dept Fis Teor, C-XI, E-28049 Madrid, Spain. RI Barrado Navascues, David/C-1439-2017 OI Barrado Navascues, David/0000-0002-5971-9242 NR 50 TC 57 Z9 57 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2001 VL 546 IS 2 BP 1006 EP 1018 DI 10.1086/318283 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393GH UT WOS:000166460500033 ER PT J AU Miller, JM Fox, DW Di Matteo, T Wijnands, R Belloni, T Pooley, D Kouveliotou, C Lewin, WHG AF Miller, JM Fox, DW Di Matteo, T Wijnands, R Belloni, T Pooley, D Kouveliotou, C Lewin, WHG TI Relativistic iron emission and disk reflection in galactic microquasar XTE J1748-288 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; line : profiles; relativity; X-rays : bursts; X-rays : stars ID RAY TIMING EXPLORER; BLACK-HOLE; SPECTRAL EVOLUTION; CYGNUS X-1; QUIESCENCE; LINE; MCG-6-30-15; OUTBURST; GALAXY; STATE AB We report evidence for an Fe K alpha fluorescence line feature and disk reflection in the very high, high-, and low-state X-ray spectra of the Galactic microquasar XTE J1748-288 during its 1998 June outburst. Spectral analyses are made on data gathered throughout the outburst by the Rossi X-Ray Timing Explorer Proportional Counter Array. Gaussian line, relativistic disk emission line, and ionized disk reflection models are fitted to the data. In the very high state the line profile appears strongly redshifted, consistent with disk emission from the innermost stable orbits around a maximally rotating Kerr black hole. In the high state the line profile is less redshifted and increasingly prominent. The low-state line profile is very strong (similar to0.5 keV equivalent width) and centered at 6.7 +/- 0.10 keV; disk line emission model fits indicate that the inner edge of the disk fluctuates between similar to 20Rg and similar to 100Rg in this state. The disk reflection fraction is traced through the outburst; reflection from an ionized disk is preferred in the very high and high states, and reflection from a relatively neutral disk is preferred in the low state. We discuss the implications of our findings for the binary system dynamics and accretion flow geometry in XTE J1748-288. C1 MIT, Dept Phys, Space Res Ctr, Cambridge, MA 02139 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron Brera, I-20121 Milan, Italy. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Miller, JM (reprint author), MIT, Dept Phys, Space Res Ctr, Cambridge, MA 02139 USA. NR 53 TC 35 Z9 35 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2001 VL 546 IS 2 BP 1055 EP 1067 DI 10.1086/318291 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393GH UT WOS:000166460500037 ER PT J AU Jain, RK Bailyn, CD Orosz, JA McClintock, JE Sobczak, GJ Remillard, RA AF Jain, RK Bailyn, CD Orosz, JA McClintock, JE Sobczak, GJ Remillard, RA TI Optical observations of the black hole candidate XTE J1550-564 during reflare and quiescence SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; stars : individual (XTE J1550-564); X-rays : stars ID TIME-SERIES ANALYSIS; X-RAY TRANSIENTS; SPECTRAL-ANALYSIS; SPACED DATA; INSTABILITY; NOVAE; MODEL AB We report optical monitoring of the soft X-ray transient XTE J1550-564 during the 1999 season (1999 January 4-August 24). The first optical observations available in 1999 show that the peak "reflare" brightness had exceeded the peak brightness of the initial optical flare in 1998 September by over half a magnitude. We compare the optical reflare light curves with the total X-ray flux, the power-law flux, and disk flux light curves constructed from the spectral fits to RXT E/PCA data. During the first 60 days of the observed optical reflare, we find no correspondence between the thermal component of the X-rays often associated with a disk and the optical flux-the former remains essentially flat, whereas the latter declines exponentially and exhibits three substantial dips. However, the power-law flux is anticorrelated with the optical dips, suggesting that the optical flux may be up scattered into the X-ray by the hot corona. Periodic modulations were discovered during the final stage of the outburst (May-June), with P = 1.546 +/- 0.038 days, and during quiescence (July and August), with P = 1.540 +/- 0.008 days. The analysis of the combined data set reveals a strong signal for a unique period at P = 1.541 +/- 0.009 days, which we believe to be the orbital period. C1 Yale Univ, Dept Phys, New Haven, CT 06520 USA. Yale Univ, Dept Astron, New Haven, CT 06520 USA. Univ Utrecht, Sterrekundig Inst, NL-3508 TA Utrecht, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Jain, RK (reprint author), Yale Univ, Dept Phys, POB 208120, New Haven, CT 06520 USA. NR 45 TC 27 Z9 27 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2001 VL 546 IS 2 BP 1086 EP 1097 DI 10.1086/318285 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393GH UT WOS:000166460500040 ER PT J AU Kaaret, P Marshall, HL Aldcroft, TL Graessle, DE Karovska, M Murray, SS Rots, AH Schulz, NS Seward, FD AF Kaaret, P Marshall, HL Aldcroft, TL Graessle, DE Karovska, M Murray, SS Rots, AH Schulz, NS Seward, FD TI Chandra observations of the young pulsar PSR B0540-69 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : general; pulsars : individual (PSR 0540-69); stars : neutron; supernova remnants; X-rays : stars ID LARGE MAGELLANIC CLOUD; GINGA OBSERVATIONS; PSR-0540-69; CALIBRATION AB The young pulsar PSR B0540-69 was one of the first targets observed with the Chandra X-Ray Observatory. The high angular resolution of Chandra allows us to resolve the compact nebula surrounding the pulsar. We have determined a position for PSR B0540-69 of R.A. = 05(h)40(m)11(s).221, decl. = -69 degrees 19'54." 98 (J2000) with a 1 sigma radial uncertainty 0."7. Combining our measurements of the pulsar period with previous measurements covering a span of 12 years, we derive a braking index of 2.082 +/- 0.005 (95% confidence). The spectrum of the pulsed emission is consistent with a power law with a photon index of 1.83 +/- 0.13. The compact nebula has a softer spectrum with a photon index of 1.85-2.26. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Kaaret, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 31 TC 47 Z9 47 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2001 VL 546 IS 2 BP 1159 EP 1167 DI 10.1086/318287 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393GH UT WOS:000166460500047 ER PT J AU Lovejoy, T AF Lovejoy, T TI Reel nature - America's romance with wildlife on film SO SCIENCE LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Lovejoy, T (reprint author), Smithsonian Inst, SI 463,1000 Jefferson Dr SW, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 5 PY 2001 VL 291 IS 5501 BP 50 EP 51 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 389VJ UT WOS:000166259100025 ER PT J AU Lovejoy, T Bouse, D AF Lovejoy, T Bouse, D TI Wildlife films SO SCIENCE LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Lovejoy, T (reprint author), Smithsonian Inst, SI 463,1000 Jefferson Dr SW, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 5 PY 2001 VL 291 IS 5501 BP 50 EP 51 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 389VJ UT WOS:000166259100024 ER PT J AU Briceno, C Vivas, AK Calvet, N Hartmann, L Pacheco, R Herrera, D Romero, L Berlind, P Sanchez, G Snyder, JA Andrews, P AF Briceno, C Vivas, AK Calvet, N Hartmann, L Pacheco, R Herrera, D Romero, L Berlind, P Sanchez, G Snyder, JA Andrews, P TI The CIDA-QUEST large-scale survey of Orion OB1: Evidence for rapid disk dissipation in a dispersed stellar population SO SCIENCE LA English DT Article ID EMISSION-LINE STARS; T TAURI PROBLEM; X-RAY; MOLECULAR CLOUD; REGION; ASSOCIATION; NEBULA AB We are conducting a large-scale, multiepoch, optical photometric survey [Centro de Investigaciones de Astronomia-Quasar Equatorial Survey Team (CIDA-QUEST)] covering about 120 square degrees to identify the young low-mass stars in the Orion OB1 association. We present results for an area of 34 square degrees. Using photometric variability as our main selection criterion, as well as follow-up spectroscopy, we confirmed 168 previously unidentified pre-main sequence stars that are about 0.6 to 0.9 times the mass of the sun (M(.)), with ages of about 1 million to 3 million years (Ori OB1b) and about 3 million to 10 million years (Ori OB1a). The Low-mass stars are spatially coincident with the high-mass (at Least 3 M(.)) members of the associations. Indicators of disk accretion such as H alpha emission and near-infrared emission from dusty disks fall sharply from Ori OB1b to Ori OB1a, indicating that the time scale for disk dissipation and possibly the onset of planet formation is a few million years. C1 Ctr Invest Astron, Merida 5101A, Venezuela. Yale Univ, Dept Astron, New Haven, CT 06511 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Los Andes, Dept Phys, Merida 5101, Venezuela. Yale Univ, Dept Phys, New Haven, CT 06520 USA. RP Briceno, C (reprint author), Ctr Invest Astron, Apartado Postal 264, Merida 5101A, Venezuela. EM briceno@cida.ve NR 40 TC 94 Z9 94 U1 0 U2 4 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 5 PY 2001 VL 291 IS 5501 BP 93 EP 96 DI 10.1126/science.291.5501.93 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 389VJ UT WOS:000166259100039 PM 11141553 ER PT J AU Thi, WF Blake, GA van Dishoeck, EF van Zadelhoff, GJ Horn, JMM Becklin, EE Mannings, V Sargent, AI van den Ancker, ME Natta, A AF Thi, WF Blake, GA van Dishoeck, EF van Zadelhoff, GJ Horn, JMM Becklin, EE Mannings, V Sargent, AI van den Ancker, ME Natta, A TI Substantial reservoirs of molecular hydrogen in the debris disks around young stars SO NATURE LA English DT Article ID MAIN-SEQUENCE STARS; SYSTEMS; SEARCH; DUST; GAS; INTERSTELLAR; EMISSION; AGE; H-2 AB Circumstellar accretion disks transfer matter from molecular clouds to young stars and to the sites of planet formation. The disks observed around pre-main-sequence stars have properties consistent with those expected for the pre-solar nebula from which our own Solar System formed 4.5 Gyr ago(1). But the 'debris' disks that encircle more than 15% of nearby main-sequence stars(2-5) appear to have very small amounts of gas, based on observations of the tracer molecule carbon monoxide(6-8) : these observations have yielded gas/dust ratios much less than 0.1, whereas the interstellar value is about 100 (ref. 9). Here we report observations of the lowest rotational transitions of molecular hydrogen (H-2) that reveal large quantities of gas in the debris disks around the stars beta Pictoris, 49 Ceti and HD135344. The gas masses calculated from the data are several hundreds to a thousand times greater than those estimated from the CO observations, and yield gas/dust ratios of the same order as the interstellar value. C1 CALTECH 15021, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA. CALTECH 10524, Div Phys Math & Astron, Pasadena, CA 91125 USA. Leiden Observ, NL-2300 RA Leiden, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP Blake, GA (reprint author), CALTECH 15021, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RI van Zadelhoff, Gerd-Jan/K-6283-2013 NR 29 TC 95 Z9 95 U1 0 U2 6 PU MACMILLAN PUBLISHERS LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 4 PY 2001 VL 409 IS 6816 BP 60 EP 63 DI 10.1038/35051033 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 388HT UT WOS:000166175600036 PM 11343110 ER PT J AU Smak, JI AF Smak, JI TI V Sge: a hot, peculiar binary system SO ACTA ASTRONOMICA LA English DT Article DE binaries : eclipsing; novae, cataclysmic variables; X-rays : stars; stars : individual : V Sge ID CATACLYSMIC VARIABLES; UV SPECTROSCOPY; ORBITAL PERIOD; SAGITTAE; ULTRAVIOLET; LIGHT; STAR; EXTINCTION; EVOLUTION; CURVES AB Five sets of mean UBV light curves of V Sge covering 2 mag of its large scale variations are analyzed. The mass ratio adopted in the analysis q = M-2/M-1 = 3.76 is that obtained by Herbig et al. (1965) from radial velocity curves based on fluorescent O III lines (arising from the surfaces of the two components). Models with an accretion disk around the white dwarf primary (or a very massive neutron star secondary) fail completely to reproduce the shapes of the observed light curves. Successful solutions are obtained with a model involving contact configuration, modified by the presence of a hot, gaseous envelope (needed to explain the behavior of colors and the variable depth of the primary eclipse). Ar inclination i approximate to 71 degrees the resulting masses of the components are: M-1 approximate to 0.9 M-circle dot and M2 approximate to 3.3 M-circle dot. In the faintest state the secondary is a main sequence star with R-2 approximate to 1.2 R-circle dot and T-2 approximate to 12 000 K, while the main parameters of the primary are: R-1 approximate to 2.1 R-circle dot. T-1 approximate to 70 000 K, and L-1 approximate to 1 x 10(38) erg/s. Due to the high radiation pressure from the primary an expanding gaseous envelope is formed, leading to the mass outflow from the system. Large scale variations involve significant increase of the temperatures of both components, up to about 140 000 K for the primary and about 50 000 K for the secondary, and a considerable thickening of the gaseous envelope, which contributes up to 20-30% of the total UBV flux. These variations are interpreted as being due - in part - to the instability and large variations in the rate of mass outflow from the secondary. No obvious explanation, however, is offered for the major increase of the temperature and luminosity of the primary component in the brightest state. The temperature of the primary in the faint and intermediate states (T-1 approximate to 70 000 K) is too low to explain the supersoft X-ray flux (observed only during those states), the only alternative being that it must come from the envelope surrounding the two stellar components. Such a hypothesis can also explain the origin of the O III and O VI lines. The distance and interstellar reddening, resulting from the solution, are d = 4 kpc and EB-V approximate to 0.30-0.36 mag. The far ultraviolet fluxes, calculated with model parameters obtained from the solution, do not agree with the observed IUE fluxes, corrected for interstellar extinction using the standard extinction law. The agreement becomes satisfactory, however, when arbitrarily chosen examples of non-standard extinction curves are used instead. C1 Polish Acad Sci, N Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. Pedag Acad, Mt Suhora Observ, PL-30084 Krakow, Poland. RP Smak, JI (reprint author), Polish Acad Sci, N Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. NR 46 TC 9 Z9 9 U1 0 U2 1 PU COPERNICUS FOUNDATION POLISH ASTRONOMY PI WARSAW PA AL UJAZDOWSKIE 4, 00-478 WARSAW, POLAND SN 0001-5237 J9 ACTA ASTRONOM JI Acta Astron. PY 2001 VL 51 IS 2 BP 117 EP 150 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 448ZF UT WOS:000169659300004 ER PT B AU van Ballegooijen, AA AF van Ballegooijen, AA BE Sigwarth, M TI Advanced solar polarimetry theory observation, and instrumentation SO ADVANCED SOLAR POLARIMETRY: THEORY, OBSERVATION, AND INSTRUMENTA TION SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 20th International National-Solar-Obervatory/Sacramento Peak Summer Workshop on Advanced Solar Polarimetry Theory, Observation, and Instrumentation CY SEP 11-15, 2000 CL NATL SOLAR OBERVAT, SUNSPOT, NM SP Natl Sci Fdn, Div Astron & Atmospher Sci, NASA, Off Space Sci, Air Force Sci Res, European Off Aerosp Res & Dev, Asian Off Aerosp Res & Dev HO NATL SOLAR OBERVAT ID MAGNETIC-FIELD AB The Advanced Solar Polarimetry workshop focussed on recent developments in spectropolarimetry and the measurement of solar magnetic fields using the Zeeman and Hanle effects. Recent results from polarimetric observations were presented and new instrument concepts were described. The workshop included sessions on instrumentation, scattering polarization, infrared polarimetry, the physics of active regions, MHD simulations, coronal magnetic fields, high resolution polarimetry, and the analysis of Stokes profiles. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van Ballegooijen, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-073-0 J9 ASTR SOC P PY 2001 VL 236 BP 1 EP 6 PG 6 WC Engineering, Aerospace; Spectroscopy SC Engineering; Spectroscopy GA BU41F UT WOS:000175937600001 ER PT B AU van Ballegooijen, AA AF van Ballegooijen, AA BE Sigwarth, M TI Three-dimensional modeling of coronal magnetic fields SO ADVANCED SOLAR POLARIMETRY: THEORY, OBSERVATION, AND INSTRUMENTA TION SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 20th International National-Solar-Obervatory/Sacramento Peak Summer Workshop on Advanced Solar Polarimetry Theory, Observation, and Instrumentation CY SEP 11-15, 2000 CL NATL SOLAR OBERVAT, SUNSPOT, NM SP Natl Sci Fdn, Div Astron & Atmospher Sci, NASA, Off Space Sci, Air Force Sci Res, European Off Aerosp Res & Dev, Asian Off Aerosp Res & Dev HO NATL SOLAR OBERVAT ID FILAMENT CHANNELS; QUIESCENT PROMINENCES; SOLAR PROMINENCES; FLUX TRANSPORT; CHIRALITY; PATTERNS; HELICITY; SUN; SUPPORT; SCALE AB The coronal magnetic field evolves in response to motions of the photospheric footpoints of coronal field lines. These motions include the effects of the solar differential rotation, meridional flows, and supergranular diffusion. Simulations have shown that these flows can lead to the formation of highly sheared or helical magnetic fields in the corona. Here we review recent modeling of such non-potential magnetic structures, and we discuss the relevance of these models to observations of filaments and prominences. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van Ballegooijen, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 37 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-073-0 J9 ASTR SOC P PY 2001 VL 236 BP 235 EP 243 PG 9 WC Engineering, Aerospace; Spectroscopy SC Engineering; Spectroscopy GA BU41F UT WOS:000175937600026 ER PT S AU Hamel, JF Conand, C Pawson, DL Mercier, A AF Hamel, JF Conand, C Pawson, DL Mercier, A BE Southward, AJ Tyler, PA Young, CM Fuiman, LA TI The sea cucumber Holothuria scabra (Holothuroidea : Echinodermata): Its biology and exploitation as beche-de-mer SO ADVANCES IN MARINE BIOLOGY, VOL 41 SE Advances in Marine Biology LA English DT Review ID CYCLE; AGENTS C1 SEVE, Katevale, PQ J0B 1W0, Canada. Univ La Reunion, Lab Ecol Marine, St Denis 97715 9, Reunion. Smithsonian Inst, Museum Natl Hist Nat, Washington, DC 20560 USA. ICLARM, Coastal Aquaculture Ctr, Honiara, Solomon Islands. ISMER, Rimouski, PQ G5L 3A1, Canada. RP Hamel, JF (reprint author), SEVE, 655 Rue Riviere, Katevale, PQ J0B 1W0, Canada. EM seve@sympatico.ca RI Mercier, Annie/B-4254-2012 NR 360 TC 64 Z9 70 U1 3 U2 27 PU ACADEMIC PRESS LTD-ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL ROAD, LONDON NW1 7DX, ENGLAND SN 0065-2881 BN 0-12-026141-3 J9 ADV MAR BIOL JI Adv. Mar. Biol. PY 2001 VL 41 BP 129 EP 223 DI 10.1016/S0065-2881(01)41003-0 PG 95 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BS95Q UT WOS:000171491400002 ER PT S AU Brown, JL Graham, LH Wielebnowski, N Swanson, WF Wildt, DE Howard, JG AF Brown, JL Graham, LH Wielebnowski, N Swanson, WF Wildt, DE Howard, JG BE Concannon, PW England, GCW Farstad, W LindeForsberg, C Verstegen, JP Doberska, C TI Understanding the basic reproductive biology of wild felids by monitoring of faecal steroids SO ADVANCES IN REPRODUCTION IN DOGS, CATS AND EXOTIC CARNIVORES SE JOURNAL OF REPRODUCTION AND FERTILITY, SUPPLEMENTS LA English DT Proceedings Paper CT 4th International Symposium on Canine and Feline Reproduction CY JUN 29-JUL 01, 2000 CL OSLO, NORWAY SP Natl Ctr Vet Contract Res & Commercial Serv Ltd, Norwegian Small Anim Vet Assoc, Norwegian Kennel Club, Premium Pet Products ID CHEETAH ACINONYX-JUBATUS; INTRAUTERINE ARTIFICIAL-INSEMINATION; NORTH-AMERICAN ZOOS; DOMESTIC CAT; OVARIAN ACTIVITY; ADRENOCORTICAL FUNCTION; CHORIONIC-GONADOTROPIN; METABOLITE ANALYSIS; SEXUAL-BEHAVIOR; LUTEAL FUNCTION AB The ability to track gonadal activity is essential for understanding the fundamentals of reproduction. Faecal steroid metabolite monitoring is a well established tool for evaluating reproductive processes in diverse mammalian species, including felids. Domestic cats were used as a model and injection of radiolabelled oestradiol, progesterone, testosterone and cortisol revealed that > 85% of metabolites were excreted in faeces with a time lag of 12-24 h. Steroids were extracted by boiling faecal material (wet or dry) in 90% aqueous ethanol followed by immunoassay with group-specific antibodies that crossreact with excreted metabolites. This approach was used to illustrate the diversity of oestrous cycle characteristics, gonadal responses to photoperiod and ovulatory sensitivity within the felid taxon. Longitudinal analyses demonstrated that faecal oestradiol increases with observed oestrus, and that the duration of the oestrous cycle varies among felid species. Seasonality in gonadal activity was observed in some species (for example clouded leopard, Pallas' cat), whereas other species (for example margay, cheetah, oncilla) are cyclic all year round. Although cats are considered induced ovulators, non-mating and spontaneous ovulation occurred in some species (for example domestic cat, clouded leopard, lion, leopard, margay) with varying frequency. There was also evidence that suppressed ovarian activity and oestrus occurred in group-housed cats (for example cheetahs). As assisted reproductive techniques, such as artificial insemination, are becoming increasingly important for managing zoo species, steroid metabolite monitoring has been especially useful for examining the efficacy of associated hormonal therapies. Exogenous gonadotrophins used to induce ovulation often caused ovarian hyperstimulation, which resulted in a maternal endocrine environment that differed from that of naturally mated cats. Finally, there is evidence that the adrenal status of animals managed under different husbandry conditions can be assessed non-invasively, thereby enhancing our understanding of how social and environmental factors affect animal well-being and reproductive fitness. In summary, understanding the basic endocrinology of endangered felids generates knowledge that can be used to improve management strategies. Because of its enormous utility and non-invasive nature, faecal hormone monitoring is one of the most powerful tools available in zoo research today. C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Brown, JL (reprint author), Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA 22630 USA. NR 52 TC 34 Z9 35 U1 5 U2 38 PU JOURNALS REPRODUCTION & FERTILITY LTD PI CAMBRIDGE PA 22 NEWMARKET RD, CAMBRIDGE CB5 8DT, ENGLAND SN 0449-3087 BN 0-906545-37-4 J9 J REP FER S PY 2001 IS 57 BP 71 EP 82 PG 12 WC Veterinary Sciences SC Veterinary Sciences GA BS21Q UT WOS:000169103800011 PM 11787193 ER PT S AU Wildt, DE Ellis, S Howard, JG AF Wildt, DE Ellis, S Howard, JG BE Concannon, PW England, GCW Farstad, W LindeForsberg, C Verstegen, JP Doberska, C TI Linkage of reproductive sciences: from 'quick fix' to 'integrated' conservation SO ADVANCES IN REPRODUCTION IN DOGS, CATS AND EXOTIC CARNIVORES SE JOURNAL OF REPRODUCTION AND FERTILITY, SUPPLEMENTS LA English DT Proceedings Paper CT 4th International Symposium on Canine and Feline Reproduction CY JUN 29-JUL 01, 2000 CL OSLO, NORWAY SP Natl Ctr Vet Contract Res & Commercial Serv Ltd, Norwegian Small Anim Vet Assoc, Norwegian Kennel Club, Premium Pet Products ID CHEETAH ACINONYX-JUBATUS; ARTIFICIAL-INSEMINATION; OVARIAN ACTIVITY; DOMESTIC CAT; INDUCTION; INVITRO; FERTILIZATION; SPERMATOZOA; OVULATION; EJACULATE AB Our laboratory has experienced four phases in understanding how the reproductive sciences contribute to genuine conservation of biodiversity. The first is the 'quick fix phase' in which the erroneous assumption is made that extant knowledge and techniques are readily adaptable to an unstudied wild animal to produce offspring rapidly. The second is the 'species-specificity phase' in which it is recognized that every species has evolved unique reproductive mechanisms that must be mastered before propagation can be enhanced. The third is the 'applicability phase' in which one grasps that all the new knowledge and technology are of minimal relevance without the cooperation of wildlife managers. The final phase is 'integration', the realization that reproduction is only one component in an abundantly complex conservation puzzle that requires interweaving many scientific disciplines with elaborate biopolitical, economic and habitat variables. These phases are illustrated using 20 years of experience with wildlife species, including the cheetah, black-footed ferret and giant panda. We conclude that the foremost value of the reproductive sciences for conserving endangered species is the discipline's powerful laboratory tools for understanding species-specific reproductive mechanisms. Such scholarly information, when applied holistically, can be used to improve management by natural or, occasionally, assisted breeding. Genuine conservation is achieved only when the reproductive knowledge and technologies are integrated into multidisciplinary programmes that preserve species integrity ex situ and preferably in situ. C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22657 USA. RP Wildt, DE (reprint author), Smithsonian Inst, Conservat & Res Ctr, Natl Zoolog Pk, Front Royal, VA 22657 USA. NR 48 TC 38 Z9 40 U1 2 U2 11 PU JOURNALS REPRODUCTION & FERTILITY LTD PI CAMBRIDGE PA 22 NEWMARKET RD, CAMBRIDGE CB5 8DT, ENGLAND SN 0449-3087 BN 0-906545-37-4 J9 J REP FER S PY 2001 IS 57 BP 295 EP 307 PG 13 WC Veterinary Sciences SC Veterinary Sciences GA BS21Q UT WOS:000169103800040 PM 11787164 ER PT S AU Ivan, A Bruni, RJ Byun, K Gorenstein, P Romaine, SE AF Ivan, A Bruni, RJ Byun, K Gorenstein, P Romaine, SE BE Freund, AK Ishikawa, T Khounsary, AM Mancini, DC Michette, AG Oestreich, S TI Hard X-ray multilayers: a study of different material systems SO ADVANCES IN X-RAY OPTICS SE Proceedings of SPIE-The International Society for Optical Engineering LA English DT Proceedings Paper CT X-Ray Mirrors, Crystals, and Multilayers Conference CY AUG 02-04, 2000 CL SAN DIEGO, CA SP SPIE DE X-ray optics; graded multilayers; sputtering deposition; X-ray reflectivity ID OPTICS AB Multilayer structures with depth-graded spacing can show a high reflectivity in a broad energy passband for hard X-rays if the interface roughness/diffuseness is controlled and minimized. We present a study of several multilayer systems deposited by DC magnetron sputtering on [111] silicon wafers and superpolished fused silica substrates. The material combinations discussed are W/Si, WSi(2)/Si, W/C, Pt/C, Ni/C, Ni/B(4)C, and Mo/Si. The deposition method used was DC magnetron sputtering at low argon pressures (1.5 to 5 mT). The characterization methods used were: Atomic Force Microscopy in tapping mode, stylus profilometry, Rutherford backscattering, cross sectional TEM, and specular X-ray reflectivity (XRR) scans at 8.05 keV. Different process parameters were varied in order to optimize the interface roughness/diffuseness sigma that was measured by XRR scans. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ivan, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 64, Cambridge, MA 02138 USA. EM aivan@cfa.harvard.edu NR 14 TC 3 Z9 3 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-3790-5 J9 P SOC PHOTO-OPT INS PY 2001 VL 4145 BP 72 EP 79 DI 10.1117/12.411622 PG 8 WC Instruments & Instrumentation; Optics; Physics, Applied; Physics, Condensed Matter SC Instruments & Instrumentation; Optics; Physics GA BS06V UT WOS:000168538300010 ER PT J AU Reitsma, R Parrish, JD McLarney, W AF Reitsma, R Parrish, JD McLarney, W TI The role of cacao plantations in maintaining forest avian diversity in southeastern Costa Rica SO AGROFORESTRY SYSTEMS LA English DT Article; Proceedings Paper CT International Symposium on Multistrata Agroforestry Systems with Perennial Crops CY FEB 22-27, 1999 CL TURRIALBA, COSTA RICA DE agroecosystem; biodiversity; bird community; community similarity; Theobroma cacao; Talamanca ID SHADE COFFEE PLANTATIONS; ELEVATIONAL GRADIENT; PLANTED SHADE; RAIN-FOREST; BIRDS; CONSERVATION; MEXICO AB We conducted 600 ten-minute, fixed-radius point counts in two climatically different seasons in forest, abandoned cacao (Theobroma cacao), and managed cacao habitat from September 1997 through April 1998 in the Talamanca lowlands of Costa Rica. A total of 1,464, 1,713, and 1,708 individual birds and 130, 131, and 144 total species were detected in forest, abandoned cacao, and managed cacao, respectively. Independent of season, cacao habitats had a significantly greater number of individuals and species per point than forest. Community similarity analyses based on guild categorizations revealed a significant degree of similarity among all habitats; however, habitat affinity analyses showed cacao habitats having significantly less forest specialists than forest. A multiple linear regression model for actively managed cacao habitat using habitat and landscape variables revealed density and diversity of canopy tree species to be significantly correlated with numbers of forest specialist species detected per point. Although nearest distance to forest was negatively correlated with the number of forest specialist species per point, it was not a significant variable in the model, possibly indicating the complex and unpredictable nature of bird movements within the complex habitat mosaic of Talamanca. The present forest bird community of the Talamanca lowlands is poor in forest specialist species relative to other forested Caribbean lowland sites. The broad patterns of avifaunal distribution illustrated by our results suggest, therefore, that although cacao plantations cannot substitute for forest, they provide habitat for a large number of species which depend to some degree on forests. C1 Smithsonian Environm Res Ctr, Avian Ecol Lab, Edgewater, MD 21037 USA. RP Reitsma, R (reprint author), Smithsonian Environm Res Ctr, Avian Ecol Lab, POB 28, Edgewater, MD 21037 USA. NR 33 TC 54 Z9 61 U1 7 U2 31 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-4366 J9 AGROFOREST SYST JI Agrofor. Syst. PY 2001 VL 53 IS 2 BP 185 EP 193 DI 10.1023/A:1013328621106 PG 9 WC Agronomy; Forestry SC Agriculture; Forestry GA 504LT UT WOS:000172858700011 ER PT J AU Meggers, BJ AF Meggers, BJ TI The mystery of the Marajoara: An ecological solution SO AMAZONIANA-LIMNOLOGIA ET OECOLOGIA REGIONALIS SYSTEMAE FLUMINIS AMAZONAS LA English DT Article DE Marajoara; archeology; Marajo Island; palm starch; Amazonia; climate change ID AMAZON AB For more than a century, the beautiful pottery from artificial mounds on the island of Marajo at the mouth of the Amazon has found its way into museums and private collections in Europe and North America, as well as Brazil. Since scientific investigations began in 1948, the discrepancy between the sophistication of the culture and the low agricultural potential of the environment has become increasingly apparent. Although claims that "Marajoara settlement pattern is urban in scale," that "the population could have been up to one million people," and that the ceramic art is "one of the most highly developed in the hemisphere" are extravagant, there is no doubt that the society maintained a relatively high level of complexity during nearly 1000 years in an environment that today supports only a sparse population dedicated mainly to cattle raising. Similar levels of cultural development elsewhere on the planet are sustained either by intensive agriculture or by unusually productive wild resources. Elimination of the former focuses attention on the latter and several new lines of evidence suggest that intensive exploitation of palm starch may be the solution to the mystery of the Marajoara. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Meggers, BJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC-112, Washington, DC 20560 USA. NR 67 TC 8 Z9 8 U1 1 U2 6 PU MAX-PLANCK-INST LIMNOLOGIE PI PLON PA AG TROPENOKOLOGIE ATTN: DR. JOACHIM ADIS POSTFACH 165, D-24302 PLON, GERMANY SN 0065-6755 J9 AMAZONIANA JI Amazon.-Limnol. Oecol. Reg. Syst. Fluminis Amazon. PY 2001 VL 16 IS 3-4 BP 421 EP 440 PG 20 WC Ecology; Limnology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 501GT UT WOS:000172677500011 ER PT J AU Lellinger, DB Prado, J AF Lellinger, DB Prado, J TI The group of Adiantum gracile in Brazil and environs SO AMERICAN FERN JOURNAL LA English DT Article AB The Adiantum gracile group of Brazil and adjacent Bolivia is a natural group distinguishable from A. tetraphyllum and related species. We provide a key to the group and describe two new Brazilian species belonging to the group A. cinnamomeum and A. dawsonii. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. Inst Bot, Secao Briol & Pteridol, BR-01061970 Sao Paulo, Brazil. RP Lellinger, DB (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RI Prado, Jefferson/C-4766-2012 OI Prado, Jefferson/0000-0003-4783-3125 NR 0 TC 5 Z9 9 U1 0 U2 0 PU AMER FERN SOC INC PI WASHINGTON PA C/O DAVID B LELLINGER, SMITHSONIAN INST, BOTANY DEPT, WASHINGTON, DC 20560 USA SN 0002-8444 J9 AM FERN J JI Am. Fern J. PD JAN-MAR PY 2001 VL 91 IS 1 BP 1 EP 8 DI 10.1640/0002-8444(2001)091[0001:TGOAGI]2.0.CO;2 PG 8 WC Plant Sciences SC Plant Sciences GA 453WN UT WOS:000169939600001 ER PT J AU Billeck, WT Eubanks, EV AF Billeck, WT Eubanks, EV TI Reassessing human remains from the Plains: changes in cultural affiliation and archaeological classification brought about by repatriation documentation. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2001 SU 32 BP 40 EP 40 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408ZX UT WOS:000167358000041 ER PT J AU Bobe, R Behrensmeyer, AK AF Bobe, R Behrensmeyer, AK TI Environmental variability and the rise of the genus Homo. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2001 SU 32 BP 41 EP 41 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408ZX UT WOS:000167358000046 ER PT J AU Jones, EB Ubelaker, DH AF Jones, EB Ubelaker, DH TI Demographic analysis of the Voegtly Cemetery sample, Pittsburgh, Pennsylvania. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2001 SU 32 BP 86 EP 86 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408ZX UT WOS:000167358000221 ER PT J AU Kardash, RR AF Kardash, RR TI Nutritional stress and femoral cortical thickness among Plains Indians. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2001 SU 32 BP 88 EP 88 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408ZX UT WOS:000167358000228 ER PT J AU Mulhern, DM Ousley, SD Jones, EB AF Mulhern, DM Ousley, SD Jones, EB TI The effects of pathology on biological affiliation. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2001 SU 32 BP 110 EP 111 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408ZX UT WOS:000167358000314 ER PT J AU Ousley, S Billeck, W AF Ousley, S Billeck, W TI Assessing tribal identity in the Plains using nontraditional craniometrics (interlandmark distances). SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2001 SU 32 BP 115 EP 116 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408ZX UT WOS:000167358000333 ER PT J AU Rashidi, JS Ortner, DJ Frohlich, B Jonsdottir, B AF Rashidi, JS Ortner, DJ Frohlich, B Jonsdottir, B TI Brucellosis in Early Bronze Age Jordan and Bahrain: an analysis of possible cases of Brucella Spondylitits. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 1 Z9 1 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2001 SU 32 BP 122 EP 123 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408ZX UT WOS:000167358000360 ER PT J AU Ross, AH Ubelaker, DH Falsetti, AB AF Ross, AH Ubelaker, DH Falsetti, AB TI Biological effects of European contact: Craniofacial variation in the Americas. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Univ Florida, CA Pound Human ID Lab, Gainesville, FL USA. Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2001 SU 32 BP 127 EP 127 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408ZX UT WOS:000167358000377 ER PT J AU Ubelaker, DH Jones, EB AF Ubelaker, DH Jones, EB TI Skeletal biology of the Voegtly Cemetery sample, Pittsburgh, Pennsylvania. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Museum Natl Hist Nat, Dept Anthropol, Smithsonian Inst, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2001 SU 32 BP 152 EP 152 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408ZX UT WOS:000167358000473 ER PT J AU Wilson, JW Tykot, RH Ubelaker, DH AF Wilson, JW Tykot, RH Ubelaker, DH TI Intradental variation in stable carbon isotope ratios in human tooth enamel. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract C1 Univ Michigan, Dept Anthropol, Ann Arbor, MI 48109 USA. Univ S Florida, Dept Anthropol, Tampa, FL 33620 USA. Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2001 SU 32 BP 166 EP 166 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 408ZX UT WOS:000167358000523 ER PT J AU Insley, SJ AF Insley, SJ TI Mother-Offspring vocal recognition in northern fur seals is mutual but asymmetrical SO ANIMAL BEHAVIOUR LA English DT Article ID HARBOR SEAL; LIONS; VOCALIZATIONS; SEPARATION AB During the 4-month period of offspring dependence, northern fur seal, Callorhinus ursinus, mothers and pups use a well-developed multimodal recognition ability to routinely find one another within large and dense breeding aggregations. I studied the vocal/auditory aspect of this ability to look at operational differences between the two members of a recognition dyad. If parent-offspring conflict theory is applied to animal communication behaviour, we should expect unequal selective forces acting on parents and offspring. In northern fur seal maternal recognition dyads, I expected pups to expend more energy in the reunion process because they carry the greater burden of a failed reunion. Furthermore, in terms of signal detection theory, pups should have a lower rejection threshold (lower bias) than mothers. To address these questions, I conducted vocal playback experiments and behavioural observations on a natural population of northern fur seals in the Pribilof Islands, Alaska, U.S.A. Although playback results support mutual vocal recognition, pups were both more vocally responsive and made more recognition errors (i.e. false alarms). Behavioural observations, including search time, distance travelled, signalling behaviour and contact with nonoffspring show that pups expend more effort in the reunion process. These findings are consistent with expectations and begin to quantify how selection pressure on recognition behaviour can vary at different stages of development. (C) 2001 The Association for the study of Animal Behaviour. C1 Univ Calif Davis, Anim Behav Grp, Davis, CA USA. Smithsonian Inst, Dept Zool Res, Washington, DC 20560 USA. RP Insley, SJ (reprint author), Hubbs SeaWorld Res Ctr, 2595 Ingraham St, San Diego, CA 92120 USA. NR 48 TC 62 Z9 63 U1 1 U2 13 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD JAN PY 2001 VL 61 BP 129 EP 137 DI 10.1006/anbe.2000.1569 PN 1 PG 9 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 410RH UT WOS:000167452600013 ER PT J AU Zatwarnicki, T Mathis, WN AF Zatwarnicki, T Mathis, WN TI A generic classification of the tribe Discocerinini (Diptera : Ephydridae) SO ANNALES ZOOLOGICI LA English DT Article DE Diptera; Ephydridae; Discocerinini; Galaterina; Orasiopa; new genera; phylogeny; taxonomy AB Broad descriptions of the genera of Discocerinini are provided for the first time. Two new genera are described: Galaterina with type species G. noonadan sp. nov. from Papuan Region and Orasiopa with type species O. millennica sp. nov. from Australasian Region. Lamproclasiopa Hendel is recognized as a genus (with Basila Cresson as its new synonym). Eleven new combinations are proposed: one in Discocerina, nine in Lamproclasiopa, one in Orasiopa. A phylogenetic reconstruction based predominantly on male terminalia is given. Eleven taxa treated as genera are grouped into three lineages. Gymnoclasiopa (most plesiomorphous, monotypic), Diclasiopa-group (intermediate with following genera: Diclasiopa, Ditrichophora, Hecamedoides, Pectinifer), and Discocerina-group (most apomorphous with following genera: Discoerina, Galarterina, Hydrochasma, Lamproclasiopa, Orasiopa, and Polytrichophora). C1 Acad Agr, Dept Zool, PL-50205 Wroclaw, Poland. Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Zatwarnicki, T (reprint author), Acad Agr, Dept Zool, Ul Cybulskiego 20, PL-50205 Wroclaw, Poland. EM zatwar@ekonom.ar.wroc.pl; Mathis.Wayne@NMNH.SI.EDU OI Zatwarnicki, Tadeusz/0000-0003-2163-0143 NR 45 TC 12 Z9 16 U1 0 U2 1 PU MUSEUM & INST ZOOLOGY PAS-POLISH ACAD SCIENCES PI WARSAW PA WILCZA STREET 64, 00-679 WARSAW, POLAND SN 0003-4541 J9 ANN ZOOL JI Ann. Zool. PY 2001 VL 51 IS 1 BP 5 EP 51 PG 47 WC Entomology SC Entomology GA 416BG UT WOS:000167759000002 ER PT J AU Barker, NP Clark, LG Davis, JI Duvall, MR Guala, GF Hsiao, C Kellogg, EA Linder, HP Mason-Gamer, RJ Mathews, SY Simmons, MP Soreng, RJ Spangler, RE AF Barker, NP Clark, LG Davis, JI Duvall, MR Guala, GF Hsiao, C Kellogg, EA Linder, HP Mason-Gamer, RJ Mathews, SY Simmons, MP Soreng, RJ Spangler, RE CA Grass Phylogeny Working Grp TI Phylogeny and subfamilial classification of the grasses (Poaceae) SO ANNALS OF THE MISSOURI BOTANICAL GARDEN LA English DT Review DE cereals; classification; DNA sequence data; evolution; grass; phylogeny; Poaceae ID INFERRING COMPLEX PHYLOGENIES; NUCLEAR RIBOSOMAL DNA; RBCL SEQUENCE DATA; PLASTID GENE RBCL; FAMILY POACEAE; NUCLEOTIDE-SEQUENCE; CHLOROPLAST DNA; COMPARATIVE MORPHOLOGY; ARUNDINOIDEAE POACEAE; MOLECULAR PHYLOGENY AB A large collaborative effort has yielded a comprehensive study of the phylogeny and a new subfamilial classification of the grass family (Poaceae/Gramineae). The study wa,, conducted oil all integrated and representative set of 62 grasses (0.6% of the species and ca. 8% of the genera) plus four outgroup taxa using six molecular sequence data sets (ndhF. rbcL, rpoC2, phyB, ITS2, and GBSS1 or waxy), chloroplast restriction site data, and morphological data. A parsimony analysis using 21.13 informative characters (the combined analysis) resulted in a single most parsimonious tree 8752 step., with all RI of 0.556 and bootstrap Support of > 90% for more than half of the internal nodes. Significant relationships that appear consistently in all analyses of all data sets and are strongly supported by the combined analysis include the following: Joinvilleaceae are sister to a monophyletic Poaceae: the earliest diverging lineages of the Poaceae are Anomochlooideae. Pharoideae, and Puelioideae, respectively: and all remaining grasses form a clade. Multiple monophyletic clades were recovered, including Bambusoideae s. str., Ehrhartoideae, Pooideae s.l., Aristidoideae, Danthonioideae, Chloridoideae s. str., Chloridoideae s.l., Panicoideae, Parianeae, Olyreae s. str.. Oryzeae, Stipeae, Meliceae, Lygeum + Nardus, and Molinia + Phragmites. The PACCAD Clade is monophyletic, containing Aristidoideae, Danthonioideae. Arundinoideae s. str., Chloridoideae s.l.. Centothecoideae, Panicoideae. Eriachne, Micraira,and Gynerium. Based on the phylogeny, a classification of 11 previously published subfamilies (Anomochlooideae, Pharoideae, Puelioideae, Bambusoideae, Ehrhartoideae, Pooideae, Aristidoideae, Arundinoideae. Chloridoideae,Centothecoideae, and Panicoideae) and 1 new subfamily (Danthonioideae) is proposed. Several changes in the circumscription of traditionally recognized subfamilies are included. Previous phylogenetic work and classifications are reviewed in relation to this classification and circumscription, and major characteristics of each subfamily are discussed and described. The matrix, trees, and updated data matrix are available at (http://www.virtualherbarium.org/grass/gpwg/ default.htm). C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Inst Systemat Bot, CH-8008 Zurich, Switzerland. Rhodes Univ, Dept Bot, ZA-6140 Grahamstown, South Africa. Iowa State Univ Sci & Technol, Dept Bot, Ames, IA 50011 USA. Cornell Univ, Mann Lib 462, LH Bailey Hortorium, Ithaca, NY 14853 USA. No Illinois Univ, Dept Biol Sci, De Kalb, IL 60115 USA. Fairchild Trop Garden, Miami, FL 33156 USA. Univ Idaho, Dept Biol Sci, Moscow, ID 83841 USA. Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. Ohio State Univ Herbarium, Columbus, OH 43212 USA. Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. RP Kellogg, EA (reprint author), Univ Missouri, Dept Biol, 8001 Nat Bridge Rd, St Louis, MO 63121 USA. EM tkellogg@umsl.edu RI Linder, Hans Peter/F-5316-2010; Simmons, Mark/F-7157-2013; Mathews, Sarah/A-6513-2015; Kellogg, Elizabeth/M-2845-2013 OI Simmons, Mark/0000-0003-3896-4633; Mathews, Sarah/0000-0002-5518-7541; Kellogg, Elizabeth/0000-0003-1671-7447 NR 214 TC 178 Z9 201 U1 4 U2 73 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 0026-6493 J9 ANN MO BOT GARD JI Ann. Mo. Bot. Gard. PY 2001 VL 88 IS 3 BP 373 EP 457 PG 85 WC Plant Sciences SC Plant Sciences GA 475BQ UT WOS:000171142100001 ER PT J AU Kellermann, KI Moran, JM AF Kellermann, KI Moran, JM TI The development of high-resolution imaging in radio astronomy SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS LA English DT Review DE aperture synthesis; image processing; interferometry; radio imaging; VLBI ID LONG-BASELINE INTERFEROMETRY; LUNAR OCCULTATION OBSERVATIONS; X-RAY CRYSTALLOGRAPHY; QUASI-STELLAR SOURCES; 3C 273; VLBI OBSERVATIONS; BRIGHTNESS DISTRIBUTIONS; LINE INTERFEROMETRY; APERTURE SYNTHESIS; LARGE ARRAY AB Since the first radio astronomy observations in the 1930s, the angular resolution of radio telescopes has improved from tens of degrees to better than one thousandth of a second of arc. This advancement has been the result of technological innovations such as stable, sensitive, short-wavelength radio receivers, digital correlators, atomic clocks, and high-speed tape recorders, as well as the development of sophisticated image processing algorithms implemented on inexpensive, fast, digital computers. C1 Natl Radio Astron Observ, Charlottesville, VA 22903 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kellermann, KI (reprint author), Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA. EM kkellerm@nrao.edu; moran@cfa.harvard.edu NR 334 TC 20 Z9 24 U1 1 U2 7 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 2001 VL 39 BP 457 EP 509 DI 10.1146/annurev.astro.39.1.457 PG 55 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 480WU UT WOS:000171487200013 ER PT J AU Lecar, M Franklin, FA Holman, MJ Murray, NW AF Lecar, M Franklin, FA Holman, MJ Murray, NW TI Chaos in the solar system SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS LA English DT Review DE celestial mechanics; planetary dynamics; Kirkwood gaps ID SHORT-PERIOD COMETS; OUTER ASTEROID BELT; MEAN MOTION RESONANCES; JUPITER-FAMILY COMETS; KUIPER-BELT; KIRKWOOD GAP; ORIGINAL DISTRIBUTION; DYNAMICAL EVOLUTION; SECULAR RESONANCES; 3/1 COMMENSURABILITY AB The physical basis of chaos in the solar system is now better understood: In all cases investigated so far, chaotic orbits result from overlapping resonances. Perhaps the clearest examples are found in the asteroid belt. Overlapping resonances account for its Kirkwood gaps and were used to predict and find evidence for very narrow gaps in the outer belt. Further afield, about one new "short-period" comet is discovered each year. They are believed to come from the "Kuiper Belt" (at 40 AU or more) via chaotic orbits produced by mean-motion and secular resonances with Neptune. Finally, the planetary system itself is not immune from chaos. In the inner solar system, overlapping secular resonances have been identified as the possible source of chaos. For example, Mercury, in 10(12) years, may suffer a close encounter with Venus or plunge into the Sun. In the outer solar system, three-body resonances have been identified as a source of chaos, but on an even longer time scale of 10(9) times the age of the solar system. On the human time scale, the planets do follow their orbits in a stately procession, and we can predict their trajectories for hundreds of thousands of years. That is because the mavericks, with shorter instability times, have long since been ejected. The solar system is not stable; it is just old!. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Toronto, Canadian Inst Theoret Astrophys, McLennan Phys Labs, Toronto, ON M5S 1A7, Canada. RP Lecar, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mlecar@cfa.harvard.edu; murray@cita.utoronto.ca NR 103 TC 63 Z9 63 U1 0 U2 4 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 2001 VL 39 BP 581 EP 631 DI 10.1146/annurev.astro.39.1.581 PG 53 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 480WU UT WOS:000171487200016 ER PT J AU Stanley, JD AF Stanley, JD TI Dating modern deltas: Progress, problems, and prognostics SO ANNUAL REVIEW OF EARTH AND PLANETARY SCIENCES LA English DT Review DE chronostratigraphy; Holocene; radiocarbon; sea-level change; sediment storage ID SEA-LEVEL RISE; RHONE CONTINENTAL-SHELF; FRASER-RIVER DELTA; NILE-DELTA; SEQUENCE STRATIGRAPHY; DEPOSITIONAL PATTERNS; MISSISSIPPI DELTA; MARINE SAMPLES; AMAZON RIVER; SEDIMENTS AB Radiocarbon dating is the method most frequently used to date Holocene deltaic sequences, but less than one quarter of C-14 dates are within +/- 500 years of predicted age. Such dates tend to be unreliable, in other words, often too old and commonly inverted upsection, and core sample dates obtained near deltaic plain surfaces may be as old as mid- to late Holocene. Stratigraphic irregularities result primarily from downslope reworking of upland alluvial sediment, with displacement of "old carbon" in the sediment that accumulates in lower valleys and deltaic plains. Use of dates that are too old results in inaccurately calculated rates (most often too low) of relative sealevel rise and/or land subsidence. More reliable timing of deltaic sediment requires a multiple-method dating approach, including, where possible, identification of associated archaeological material. Developing an accurate dating strategy is a critical step for implementing reliable coastal protection measures needed fur the rapidly increasing human populations in these low-lying, vulnerable nearshore settings. C1 Smithsonian Inst, Natl Museum Nat Hist, Deltas Global Change Program, Washington, DC 20560 USA. RP Stanley, JD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Deltas Global Change Program, Washington, DC 20560 USA. NR 136 TC 17 Z9 18 U1 2 U2 10 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0084-6597 J9 ANNU REV EARTH PL SC JI Annu. Rev. Earth Planet. Sci. PY 2001 VL 29 BP 257 EP 294 DI 10.1146/annurev.earth.29.1.257 PG 38 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 434JF UT WOS:000168810800010 ER PT J AU DiMichele, WA Pfefferkorn, HW Gastaldo, RA AF DiMichele, WA Pfefferkorn, HW Gastaldo, RA TI Response of Late Carboniferous and Early Permian plant communities to climate change SO ANNUAL REVIEW OF EARTH AND PLANETARY SCIENCES LA English DT Review DE ecosystem stability; glaciation; biome; coal; extinction ID CENTRAL APPALACHIAN BASIN; LATE PALEOZOIC GLACIATION; COAL-SWAMP VEGETATION; NORTH-AMERICA; PALEOCLIMATE CONTROLS; EASTERN KENTUCKY; ILLINOIS BASIN; PEAT FORMATION; WARRIOR BASIN; WEST-VIRGINIA AB Late Carboniferous and Early Permian strata record the transition from a cold interval in Earth history, characterized by the repeated periods of glaciation and deglaciation of the southern pole, to a warm-climate interval. Consequently, this time period is the best available analogue to the Recent in which to study patterns of vegetational response, both to glacial-interglacial oscillation and to the appearance of warm climate. Carboniferous wetland ecosystems were dominated by spore-producing plants and early gymnospermous seed plants. Global climate changes, largely drying, forced vegetational changes, resulting in a change to a seed plant-dominated world, beginning first at high latitudes during the Carboniferous, reaching the tropics near the Permo-Carboniferous boundary. For most of this time plant assemblages were very conservative in their composition. Change in the dominant vegetation was generally a rapid process, which suggests that environmental thresholds were crossed, and involved little mixing of elements from the wet and dry floras. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA. Colby Coll, Dept Geol, Waterville, ME 04901 USA. RP DiMichele, WA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RI DiMichele, William/K-4301-2012 NR 173 TC 111 Z9 116 U1 2 U2 30 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0084-6597 J9 ANNU REV EARTH PL SC JI Annu. Rev. Earth Planet. Sci. PY 2001 VL 29 BP 461 EP 487 DI 10.1146/annurev.earth.29.1.461 PG 27 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 434JF UT WOS:000168810800015 ER PT J AU Levin, LA Etter, RJ Rex, MA Gooday, AJ Smith, CR Pineda, J Stuart, CT Hessler, RR Pawson, D AF Levin, LA Etter, RJ Rex, MA Gooday, AJ Smith, CR Pineda, J Stuart, CT Hessler, RR Pawson, D TI Environmental influences on regional deep-sea species diversity SO ANNUAL REVIEW OF ECOLOGY AND SYSTEMATICS LA English DT Review DE biodiversity; benthos; environmental gradients; depth gradients; diversity measures; bathyal; abyssal; sediments ID OXYGEN-MINIMUM ZONE; CAROLINA CONTINENTAL-SLOPE; NORTH-ATLANTIC NEMATODES; CORAL LOPHELIA-PERTUSA; SANTA-BARBARA BASIN; GULLMAR-FJORD BASIN; COMMUNITY STRUCTURE; ORGANIC-CARBON; BENTHIC FORAMINIFERA; PARTICLE-SIZE AB Most of our knowledge of biodiversity and its causes in the deep-sea benthos derives from regional-scale sampling studies of the macrofauna. Improved sampling methods and the expansion of investigations into a wide variety of habitats have revolutionized our understanding of the deep sea. Local species diversity shows clear geographic variation on spatial scales of 100-1000 km. Recent sampling programs have revealed unexpected complexity in community structure at the landscape level that is associated with large-scale oceanographic processes and their environmental consequences. We review the relationships between variation in local species diversity and the regional-scale phenomena of boundary constraints, gradients of productivity, sediment heterogeneity, oxygen availability, hydrodynamic regimes, and catastrophic physical disturbance. We present a conceptual model of how these interdependent environmental factors shape regional-scale variation in local diversity. Local communities in the deep sea may be composed of species that exist as metapopulations whose regional distribution depends on a balance among global-scale, landscape-scale, and small-scale dynamics. Environmental gradients may form geographic patterns of diversity by influencing local processes such as predation, resource partitioning, competitive exclusion, and facilitation that determine species coexistence. The measurement of deep-sea species diversity remains a vital issue in comparing geographic patterns and evaluating their potential causes. Recent assessments of diversity using species accumulation curves with randomly pooled samples confirm the often-disputed claim that the deep sea supports higher diversity than the continental shelf. However, more intensive quantitative sampling is required to fully characterize the diversity of deep-sea sediments, the most extensive habitat on Earth. Once considered to be constant, spatially uniform, and isolated, deep-sea sediments are now recognized as a dynamic, richly textured environment that is inextricably linked to the global biosphere. Regional studies of the last two decades provide the empirical background necessary to formulate and test specific hypotheses of causality by controlled sampling designs and experimental approaches. C1 Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. Univ Massachusetts, Dept Biol, Boston, MA 02125 USA. Southampton Oceanog Ctr, Southampton SO14 3ZH, Hants, England. Univ Hawaii, Dept Oceanog, Honolulu, HI 96822 USA. Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. EM llevin@ucsd.edu; ron.etter@umb.edu; michael.rex@umb.edu; ang@soc.soton.ac.uk; csmith@soest.hawaii.edu; jpineda@whoi.edu; carol.stuart@umb.edu; rhessler@ucsd.edu; pawson.david@nmnh.si.edu NR 214 TC 350 Z9 365 U1 20 U2 128 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4162 J9 ANNU REV ECOL SYST JI Annu. Rev. Ecol. Syst. PY 2001 VL 32 BP 51 EP 93 DI 10.1146/annurev.ecolsys.32.081501.114002 PG 43 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 505JC UT WOS:000172908800003 ER PT J AU Rubidge, BS Sidor, CA AF Rubidge, BS Sidor, CA TI Evolutionary patterns among permo-triassic therapsids SO ANNUAL REVIEW OF ECOLOGY AND SYSTEMATICS LA English DT Review DE synapsida; Therapsida; mammal-like reptile; Permian; phylogeny ID MAMMAL-LIKE REPTILE; ECCA-BEAUFORT CONTACT; SOUTH-AFRICA; KAROO BASIN; NONMAMMALIAN THERAPSIDS; ISCHIGUALASTO FORMATION; VERTEBRATE TAPHONOMY; FUNCTIONAL-ANATOMY; AMNIOTE PHYLOGENY; CRANIAL ANATOMY AB A rich fossil record documents nonmammalian evolution. In recent years, the application of cladistic methodology has shed valuable light on the relationships within the therapsid clades Biarmosuchia, Dinocephalia, Anomodontia, and Cynodontia. Recent discoveries from South Africa suggest that Gondwana, rather than Laurasia, was the center of origin and radiation for many early therapsids. Because of their relative abundance and global distribution, therapsids have enjoyed widespread use in biostratigraphy, basin analysis, and paleo-environmental and -continental reconstructions. Synapsids (including therapsids) form the bulk of tetrapod diversity (in terms of both number of species and abundance) from Early Permian to Middle Triassic times and thus can provide critical information on the nature of the Permo-Triassic extinction in the terrestrial realm. Quantitative techniques have produced headway into understanding the relative importance of homoplasy and convergent evolution in the origin of mammals. C1 Univ Witwatersrand, Bernard Price Inst Palaeontol Res, Johannesburg, South Africa. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Univ Witwatersrand, Bernard Price Inst Palaeontol Res, Johannesburg, South Africa. EM l06gar@cosmos.wits.ac.za; sidor.christian@nmnh.si.edu OI Rubidge, Bruce/0000-0003-2477-1873 NR 166 TC 91 Z9 98 U1 3 U2 25 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4162 J9 ANNU REV ECOL SYST JI Annu. Rev. Ecol. Syst. PY 2001 VL 32 BP 449 EP 480 DI 10.1146/annurev.ecolsys.32.081501.114113 PG 32 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 505JC UT WOS:000172908800016 ER PT J AU Vandiver, P AF Vandiver, P TI The role of materials research in ceramics and archaeology SO ANNUAL REVIEW OF MATERIALS RESEARCH LA English DT Review DE archaeological science; pyrotechnology; glass and glazes; plasters; craft history; ethnoarchaeology; archeomaterials; history of technology ID NEAR-EAST; BEGINNINGS; POTTERY; SCIENCE AB Materials research has been applied successfully to the study of archaeological ceramics for the last fifty years. To learn about our history and the human condition is not just to analyze and preserve the objects but also to investigate and understand the knowledge and skills used to produce and use them. Many researchers have probed the limits and methods of such studies. always mindful that a glimpse at ancient reality lies in the details of time and place, context of finds, and experimentally produced data, usually compared with standards that were collected in an equivalent ethnographic setting or that were fabricated in a laboratory in order to elucidate the critical questions in a technology that could be understood in no other way. The basis of most studies of ancient technology has been established as microstructure; composition and firing: methods and sequence of manufacture; differentiation of use: use-wear and post-depositional processes, technological variability that can be interpreted as a pattern of stasis or innovation, which can be related to cultural continuity or change; and interpretation that can involve technology, subsistence trade, organization, and symbolic group- and self-definition. C1 Smithsonian Inst, Smithsonian Ctr Mat Res & Educ, Washington, DC 20560 USA. RP Vandiver, P (reprint author), Smithsonian Inst, Smithsonian Ctr Mat Res & Educ, Washington, DC 20560 USA. NR 69 TC 10 Z9 10 U1 0 U2 9 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 1531-7331 J9 ANN REV MATER RES JI Ann. Rev. Mater. Res. PY 2001 VL 31 BP 373 EP 385 DI 10.1146/annurev.matsci.31.1.373 PG 13 WC Materials Science, Multidisciplinary SC Materials Science GA 486FX UT WOS:000171808700016 ER PT J AU Neale, PJ Bossard, P Huot, Y AF Neale, PJ Bossard, P Huot, Y TI Incident and in situ irradiance in Lakes Cadagno and Lucerne: A comparison of methods and models SO AQUATIC SCIENCES LA English DT Article; Proceedings Paper CT 7th International GAP Workshop CY SEP 09-17, 1999 CL SWITZERLAND DE Lake Lucerne; Lake Cadagno; PAR; UV-A; UV-B; irradiance regime; radiative transfer models; altitude effect ID ULTRAVIOLET-RADIATION; OZONE DEPLETION; PHYTOPLANKTON; PHOTOSYNTHESIS; VARIABILITY; ATTENUATION; PHOTOLYSIS AB Incident surface irradiance of photosynthetically available radiation (PAR), and ultraviolet radiation (UV-A and UV-B) was monitored during the GAP Workshop (8-15 September 1999) at the field stations Kastanienbaum at Lake Lucerne (434 m a.s.l.) and Piora at Lake Cadagno (1923 m a.s.l.), Switzerland, with broad band sensors (LiCOR and Macam) and multifilter spectral radiometers (Smithsonian UV-B radiometer SR18, Satlantic and Biospherical Profilers). Calculations of clear sky spectral irradiance were performed using computer implementations of atmospheric radiative transfer models STAR and FASTRT as well as a simple two-stream model. Clear sky conditions prevailed at Lucerne so that detailed comparisons could be made between measured irradiance and model predictions. Good correspondence was found for the measurements and predictions. The best agreement was with the STAR model. Spectral measurements were consistent with measurements of the broad band UV-A and UV-B sensors after accounting for the manufacturer specified spectral response. The effective center wavelength of the broad band UV-B sensor is 320 nm, despite the fact that the maximum sensitivity of the sensor is at 310 nm. A daily UV index was estimated from the midday SR18 data. An analysis of the UV-A and UV-B data at the two sites of different altitude indicates that the so called altitude effect (AE) is variable during the course of the day and usually higher for UV-B than for UV-A. Lakes Lucerne and Cadagno have moderate transparency to UV and PAR with 50% of 320 nm irradiance penetrating to 1 m in Lake Lucerne and 0.3 m in Lake Cadagno. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. EAWAG, Limnol Res Ctr, CH-6047 Kastanienbaum, Switzerland. Dalhousie Univ, Dept Oceanog, CEOTR, Halifax, NS B3H 4J1, Canada. RP Neale, PJ (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RI Neale, Patrick/A-3683-2012; Huot, Yannick/B-4497-2008; OI Huot, Yannick/0000-0003-1793-761X; Sommaruga, Ruben/0000-0002-1055-2461 NR 22 TC 17 Z9 17 U1 2 U2 7 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 1015-1621 J9 AQUAT SCI JI Aquat. Sci. PY 2001 VL 63 IS 3 BP 250 EP 264 DI 10.1007/s00027-001-8038-5 PG 15 WC Environmental Sciences; Limnology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 493CJ UT WOS:000172204200002 ER PT J AU Neale, PJ Litchman, E Sobrino, C Callieri, C Morabito, G Montecino, V Huot, Y Bossard, P Lehmann, C Steiner, D AF Neale, PJ Litchman, E Sobrino, C Callieri, C Morabito, G Montecino, V Huot, Y Bossard, P Lehmann, C Steiner, D TI Quantifying the response of phytoplankton photosynthesis to ultraviolet radiation: Biological weighting functions versus in situ measurements in two Swiss lakes SO AQUATIC SCIENCES LA English DT Article; Proceedings Paper CT 7th International GAP Workshop CY SEP 09-17, 1999 CL SWITZERLAND DE Lake Lucerne; Lake Cadagno; inhibition; primary production; UV-A; UV-B ID CARBON FIXATION; MARINE DIATOM; ARCTIC LAKES; INHIBITION; ACIDIFICATION; TEMPERATURE; EXPOSURE; DAMAGE; REPAIR AB The sensitivity of photosynthesis to ultraviolet radiation (UV) was assessed for phytoplankton assemblages in two Swiss lakes, pre-alpine Lake Lucerne (Vierwaldstattersee) and alpine Lake Cadagno, using both in situ and laboratory incubations. Biological weighting functions for UV inhibition of photosynthesis (BWFs) were determined in the laboratory using polychromatic exposures in a Xe-lamp based incubator. Samples were concurrently incubated in situ under UV exposed and protected bottles (profiles 0-5 m), while additional spectral treatments were carried out at the 50% UV-B penetration depth: full spectrum, UV-A only (Mylar protected) and UV protected quartz tubes. Both particulate (>0.2 mum) and total organic carbon incorporation were measured. Measured attenuation coefficients and incident UV spectral irradiance data was used to evaluate a BWF/photosynthesis-irradiance model (BWF/P-I) for in situ exposure conditions and compared with measurements. The BWFs showed sensitivity across the UV spectrum at similar, though somewhat lower, levels than an average BWF for marine assemblages. Relative photosynthesis in situ (UV exposed/UV excluded) was about 40% at the surface and about 60% at the 50% UV-B penetration depth. Similar inhibition was predicted by the BWF/P-I model. Generally, full spectrum (UV-B and UV-A) exposure had little additional effect compared to UV-A only exposure. Reciprocal transfer of samples between lakes showed enhancement of UV effects in L. Cadagno compared to incubation of the same sample in L. Lucerne, consistent with increased UV sensitivity due to the 5 degreesC cooler water temperature in L. Cadagno. Similarly, BWF prediction of in situ response in L. Cadagno was improved by increasing UV sensitivity according to a Q(10) of 2. Full profile calculations using the BWF/P-I model suggest stronger effects of UV on L. Lucerne compared to L. Cadagno phytoplankton due to greater sensitivity of the assemblage combined with higher overall transparency to UV relative to PAR in L. Lucerne. The BWF/P-I model was a good overall predictor of UV-dependent photosynthetic performance in these lakes. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. CSIC, Inst Ciencias Marinas Andalucia, Cadiz 11510, Spain. CNR, Ist Italiano Idrobiol, I-28922 Verbania, Italy. Univ Chile, Fac Ciencias, Santiago, Chile. Dalhousie Univ, Dept Oceanog, CEOTR, Halifax, NS B3H 4J1, Canada. EAWAG, Limnol Res Ctr, CH-6047 Kastanienbaum, Switzerland. Univ Zurich, Inst Plant Biol, CH-8008 Zurich, Switzerland. RP Neale, PJ (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RI Neale, Patrick/A-3683-2012; Huot, Yannick/B-4497-2008; Sobrino, Cristina/J-3534-2012; Morabito, Giuseppe/I-6633-2013; OI Huot, Yannick/0000-0003-1793-761X; Morabito, Giuseppe/0000-0002-8223-3259; Sobrino, Cristina/0000-0003-0431-1220 NR 38 TC 19 Z9 19 U1 1 U2 10 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 1015-1621 J9 AQUAT SCI JI Aquat. Sci. PY 2001 VL 63 IS 3 BP 265 EP 285 DI 10.1007/PL00001354 PG 21 WC Environmental Sciences; Limnology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 493CJ UT WOS:000172204200003 ER PT J AU Callieri, C Morabito, G Huot, Y Neale, PJ Litchman, E AF Callieri, C Morabito, G Huot, Y Neale, PJ Litchman, E TI Photosynthetic response of pico- and nanoplanktonic algae to UVB, UVA and PAR in a high mountain lake SO AQUATIC SCIENCES LA English DT Article; Proceedings Paper CT 7th International GAP Workshop CY SEP 09-17, 1999 CL SWITZERLAND DE UV radiation; autotrophic picoplankton; high mountain lake ID ULTRAVIOLET-RADIATION; PHYTOPLANKTON PHOTOSYNTHESIS; PICOPLANKTON; INHIBITION; ORGANISMS; IMPACT AB The objective of the present study was to evaluate the influence of UV radiation on photosynthesis rate. in situ and in laboratory incubations, on size fractionated natural algal assemblages (picoplankton: 0.2-2 mum, nanoplankton: >2 mum) and whole water (total organic carbon TOC). Near surface samples from a mesotrophic high mountain lake (LCD: L. Cadagno. Swiss Alps, Switzerland, 1923 m a.s.l.) and from the oligotrophic pre-alpine L. Lucerne (LLU: Swiss Alps, Switzerland, 434 m a.s.l.) were both incubated at a depth of 30 cm (50% of surface UV at 323 nm) in L. Cadagno. At the same time, biological weighting functions for UV inhibition of photosynthesis (BWFs) were determined for the autotrophic picoplankton and whole fraction in a spectral incubator. Photosynthetic assimilation of the pico- and nanoplanktonic algal communities as well as the assimilated total organic carbon (TOC) was estimated separately by C-14 uptake under three irradiance conditions: PAR (photosynthetically active radiation), PAR + UVA and PAR + UVA + UVB. UV radiation reduced significantly photosynthesis rate in samples from both lakes (LLU: P=0.0012; LCD: P=0.0001). It appears that UVA plus UVB significantly affect the algal assemblage in both lakes; however most of the effect is due to UVA (Mann Whitney U test, two tailed: P=0.0022). The natural assemblages from LLU transplanted to LCD were more inhibited by UV than the autochthonous assemblages of LCD. Photosynthetic rates of picoplankton from LLU and LCD under full UV exposure was reduced by 73% and 55% respectively relative to PAR only. A higher sensitivity of autotrophic picoplankton to the UV radiation, with respect to the nanoplankton, was observed in the biological weighting functions. However this difference was not statistically significant for the in situ incubations. C1 CNR, Ist Italiano Idrobiol, I-28922 Pallanza, Italy. Dalhousie Univ, Dept Oceanog, CEOTP, Halifax, NS B3H 4J1, Canada. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. EAWAG, Limnol Res Ctr, CH-6047 Kastanienbaum, Switzerland. RP Callieri, C (reprint author), CNR, Ist Italiano Idrobiol, Largo Tonolli 50, I-28922 Pallanza, Italy. RI Neale, Patrick/A-3683-2012; Huot, Yannick/B-4497-2008; Morabito, Giuseppe/I-6633-2013 OI Huot, Yannick/0000-0003-1793-761X; Morabito, Giuseppe/0000-0002-8223-3259 NR 23 TC 23 Z9 25 U1 1 U2 9 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 1015-1621 J9 AQUAT SCI JI Aquat. Sci. PY 2001 VL 63 IS 3 BP 286 EP 293 DI 10.1007/PL00001355 PG 8 WC Environmental Sciences; Limnology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 493CJ UT WOS:000172204200004 ER PT J AU Kohler, J Schmitt, M Krumbeck, H Kapfer, M Litchman, E Neale, PJ AF Kohler, J Schmitt, M Krumbeck, H Kapfer, M Litchman, E Neale, PJ TI Effects of UV on carbon assimilation of phytoplankton in a mixed water column SO AQUATIC SCIENCES LA English DT Article; Proceedings Paper CT 7th International GAP Workshop CY SEP 09-17, 1999 CL SWITZERLAND DE primary production; ultraviolet radiation; light inhibition; turbulent mixing; model ID ULTRAVIOLET-RADIATION; MARINE DIATOM; PHOTOSYNTHESIS; LAKE; SUBSEQUENT; INHIBITION; DAMAGE AB Carbon assimilation is usually measured at fairly constant light intensities. Under natural conditions, however, planktonic algae are moved through the water column and experience light of fluctuating intensity and spectral composition. They may cope with strong UV for a short residence in the upper water layer. In order to estimate the effects of UV on primary production of phytoplankton under conditions of turbulent mixing, we compared carbon assimilation and exudation of algae incubated in UV-transparent quartz and in UV-absorbing glass bottles which were moved through different water lavers. Computer-controlled elevators were used to simulate mixing depths between 2 and 14 meters. Compared to the glass bottles, particulate C assimilation in the quartz bottles was reduced by 20-30% at mixing depths between 2 and 10 m. There was no significant difference between both types of incubation bottles at a mixing depth of 14 m. Exudation was enhanced by UV near the water surface (mixing depth up to 4 m) but not in the deep-mixed samples. Our results indicate serious damage of planktonic algae by UV even under conditions of vertical mixing if the euphotic zone exceeds the mixing depth. Depression was low for circulation through the whole euphotic zone and may disappear at even deeper mixing. Our results indicate lower photoinhibition per UV dosage at fluctuating than at constant light intensities. A model predicting inhibition as function of weighted irradiance spectra was adapted to describe wavelength dependent photoinhibition occurring at different mixing depths. The model results agreed very well with the inhibition rates measured under fluctuating light. These preliminary results are used to discuss the importance of UV on photosynthesis of planktonic algae in aquatic environments of different mixing depths and stabilities of stratification. C1 Inst Freshwater Ecol & Inland Fisheries, D-12587 Berlin, Germany. UFZ Helmholtz Ctr Environm Res, D-04318 Leipzig, Germany. Tech Univ Cottbus, D-15526 Bad Saarow Pieskow, Germany. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Kohler, J (reprint author), Inst Freshwater Ecol & Inland Fisheries, Muggelseedamm 301, D-12587 Berlin, Germany. EM Koehler@igb-berlin.de RI Neale, Patrick/A-3683-2012; Kohler, Jan/C-2633-2014 NR 31 TC 22 Z9 22 U1 2 U2 5 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 1015-1621 J9 AQUAT SCI JI Aquat. Sci. PY 2001 VL 63 IS 3 BP 294 EP 309 DI 10.1007/PL00001356 PG 16 WC Environmental Sciences; Limnology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 493CJ UT WOS:000172204200005 ER PT J AU Zilczer, J AF Zilczer, J TI A not-so-peaceable kingdom: Horace Pippin's 'Holy Mountain' SO ARCHIVES OF AMERICAN ART JOURNAL LA English DT Article C1 Smithsonian Inst, Hirshhorn Museum & Sculpture Garden, Washington, DC 20560 USA. RP Zilczer, J (reprint author), Smithsonian Inst, Hirshhorn Museum & Sculpture Garden, Washington, DC 20560 USA. NR 45 TC 0 Z9 0 U1 0 U2 0 PU ARCHIVES AMER ART PI WASHINGTON PA 8TH & F STREETS, WASHINGTON, DC 20560 USA SN 0003-9853 J9 ARCH AM ART J JI Arch. Am. Art J. PY 2001 VL 41 IS 1-4 BP 18 EP + PG 0 WC Art SC Art GA 613EL UT WOS:000179119000002 ER PT J AU Mann, T AF Mann, T TI The body of Raphaelle Peale: Still life and selfhood, 1812-1824 SO ARCHIVES OF AMERICAN ART JOURNAL LA English DT Book Review C1 Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. RP Mann, T (reprint author), Smithsonian Inst, Natl Portrait Gallery, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ARCHIVES AMER ART PI WASHINGTON PA 8TH & F STREETS, WASHINGTON, DC 20560 USA SN 0003-9853 J9 ARCH AM ART J JI Arch. Am. Art J. PY 2001 VL 41 IS 1-4 BP 43 EP 46 PG 4 WC Art SC Art GA 613EL UT WOS:000179119000004 ER PT S AU Freeman, PE Doe, S Siemiginowska, A AF Freeman, PE Doe, S Siemiginowska, A BE Starck, JL Murtagh, FD TI Sherpa: a mission-independent data analysis application SO ASTRONOMICAL DATA ANALYSIS SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Astronomical Data Analysis CY AUG 02-03, 2001 CL SAN DIEGO, CA SP SPIE DE Chandra; CIAO; data analysis; fitting; modeling; Virtual Observatory AB The ever-increasing quality and complexity of astronomical data underscores the need for new and powerful data analysis applications. This need has led to the development of Sherpa, a modeling and fitting program in the CIAO software package that enables the analysis of multi-dimensional, multi-wavelength data. In this paper, we present an overview of Sherpa's features, which include: support for a wide variety of input and output data formats, including the new Model Descriptor List (MDL) format; a model language which permits the construction of arbitrarily complex model expressions, including ones representing instrument characteristics; a wide variety of fit statistics and methods of optimization, model comparison, and parameter estimation; multi-dimensional visualization, provided by ChIPS; and new interactive analysis capabilities provided by embedding the S-Lang interpreted scripting language. We conclude by showing example Sherpa analysis sessions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Freeman, PE (reprint author), Harvard Smithsonian Ctr Astrophys, MS 81,60 Garden St, Cambridge, MA 02138 USA. EM pfreeman@head-cfa.harvard.edu; sdoe@head-cfa.harvard.edu; asiemiginowska@head-cfa.harvard.edu NR 12 TC 177 Z9 177 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4191-0 J9 PROC SPIE PY 2001 VL 4477 BP 76 EP 87 DI 10.1117/12.447161 PG 12 WC Astronomy & Astrophysics; Computer Science, Artificial Intelligence; Computer Science, Information Systems SC Astronomy & Astrophysics; Computer Science GA BT68L UT WOS:000173724200008 ER PT S AU Kurtz, MJ Eichhorn, G AF Kurtz, MJ Eichhorn, G BE Starck, JL Murtagh, FD TI Evolution of Urania into the AVO SO ASTRONOMICAL DATA ANALYSIS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Astronomical Data Analysis CY AUG 02-03, 2001 CL SAN DIEGO, CA SP SPIE DE information retrieval; Astronomical Virtual Observatory C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurtz, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009; OI Eichhorn, Guenther/0000-0002-3032-1978; Kurtz, Michael/0000-0002-6949-0090 NR 1 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4191-0 J9 P SOC PHOTO-OPT INS PY 2001 VL 4477 BP 186 EP 190 DI 10.1117/12.447172 PG 5 WC Astronomy & Astrophysics; Computer Science, Artificial Intelligence; Computer Science, Information Systems SC Astronomy & Astrophysics; Computer Science GA BT68L UT WOS:000173724200019 ER PT S AU McDowell, JC AF McDowell, JC BE Starck, JL Murtagh, FD TI Data analysis with the Chandra Data Model library SO ASTRONOMICAL DATA ANALYSIS SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Astronomical Data Analysis CY AUG 02-03, 2001 CL SAN DIEGO, CA SP SPIE DE data analysis; astronomy; FITS AB The Chandra Data Model (CDM) library was developed to support data analysis for the Chandra X-ray Observatory, one of NASA's orbiting Great Observatories. The library and its associated tools are designed to be multi-mission and can be used to manipulate a wide variety of astronomical data. Much of the library's power comes from its use of 'virtual files', which provide a flexible command-line user interface. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 13 TC 2 Z9 2 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4191-0 J9 PROC SPIE PY 2001 VL 4477 BP 234 EP 240 DI 10.1117/12.447179 PG 7 WC Astronomy & Astrophysics; Computer Science, Artificial Intelligence; Computer Science, Information Systems SC Astronomy & Astrophysics; Computer Science GA BT68L UT WOS:000173724200025 ER PT S AU Morris, DC Aldcroft, TL Cameron, RA Cresitello-Dittmar, ML Karovska, M AF Morris, DC Aldcroft, TL Cameron, RA Cresitello-Dittmar, ML Karovska, M BE Starck, JL Murtagh, FD TI Analysis of the Chandra X-ray Observatory Aspect Camera PSF and its application to post-facto pointing aspect determination SO ASTRONOMICAL DATA ANALYSIS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Astronomical Data Analysis CY AUG 02-03, 2001 CL SAN DIEGO, CA SP SPIE DE Chandra; aspect; raytrace; point spread function; pointing performance AB For the last 20 months, the Chandra X-Ray Observatory (Weisskopf et. al. 2000) has been producing X-ray images of the universe in stunning detail. This is due in large part to the excellent post-facto pointing aspect determination for Chandra (Aldcroft et. al. 2000). This aspect determination performance is achieved using elliptical gaussian centroiding techniques. Application of point spread function (PSF) fitting using a true PSF model for the Aspect Camera Assembly (ACA) on Chandra could improve this performance. We have investigated the use of an ACA PSF model in the post-facto centroiding of stars and fiducial lights imaged by the ACA. We will present the methodologies explored for use in determining a model for the ACA PSF and discuss the results of a comparison of PSF fit centroiding and the current method of elliptical gaussian centroiding as they apply to post-facto aspect reconstruction. The first method of recovering the ACA PSF uses a raytrace model of the ACA to generate simulated stellar PSFs. In this method, the MACOS raytracing software package is used to describe each element of the Chandra aspect optical system. The second method investigated is the so called shift and add method whereby we build a high resolution image of the PSF by combining several thousand low resolution images of a single star collected by the ACA while tracking during normal science observations. The programmed dither of the spacecraft slowly sweeps the stellar image across the ACA focal plane, and the many slightly offset images are used to effectively increase the resolution of the resultant image of the star to a fraction of an ACA pixel. In each method, a library of PSF images is built at regularly gridded intervals across the ACA focal plane. This library is then used to interpolate a PSF at any desired position on the focal plane. We have used each method to reprocess the aspect solution of a set of archived Chandra observation and compare the results to one another and to the delivered post-facto aspect solution, currently derived using elliptical gaussian centroiding of ACA star images. Finally, we will present a summary of Chandra's aspect performance achieved to date, and discuss the effect of incorporating a PSF model into the post-facto aspect determination software. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Morris, DC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-4191-0 J9 P SOC PHOTO-OPT INS PY 2001 VL 4477 BP 254 EP 264 DI 10.1117/12.447182 PG 11 WC Astronomy & Astrophysics; Computer Science, Artificial Intelligence; Computer Science, Information Systems SC Astronomy & Astrophysics; Computer Science GA BT68L UT WOS:000173724200028 ER PT B AU Murray, SS AF Murray, SS BE Harnden, FR Primini, FA Payne, HE TI Chandra X-ray Observatory - First year science highlights SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO ID TRANSMISSION GRATING SPECTROMETER; AXAF AB The Chandra X-ray Observatory achieved orbit on July 23, 1999, and began science observing in October 1999. Now over a year since the first light image of Cas-A, Chandra has observed several hundred science targets and many calibration objects. A few highlights from these data are presented - including a discussion of the spatially resolved spectrum of supernova ejecta in Cas-A and X-ray emission from the central regions of M31, the nearby AGN Cen-A, and the quasar 3C273. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Murray, SS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 13 EP 21 PG 9 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400002 ER PT B AU Brissenden, RJ AF Brissenden, RJ BE Harnden, FR Primini, FA Payne, HE TI Chandra X-ray observatory operations SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB The Chandra X-ray Observatory was launched from the Space Shuttle on 23 July 1999 and has completed the first year of operations with outstanding results. We present a description of the Chandra Observatory, the Chandra mission operations concept, ground system architecture, selected operations metrics and an example where operational processes have required modification due to on-orbit events and experience. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brissenden, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 22 EP 31 PG 10 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400003 ER PT B AU Zhao, JH Tsutsumi, T AF Zhao, JH Tsutsumi, T BE Harnden, FR Primini, FA Payne, HE TI The submillimeter array data-handling system SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB We report on the basic design and current status of the data-handling system for the Submillimeter Array (SMA). Components of this system currently under development include the data storage format, archive, and off-line data reduction software. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhao, JH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 164 EP 167 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400037 ER PT B AU Mandel, E Murray, SS Roll, J AF Mandel, E Murray, SS Roll, J BE Harnden, FR Primini, FA Payne, HE TI Funtools: An experiment with minimal buy-in software SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB Minimal buy-in software seeks to hide from its users the complexity of complex code. This means striking a balance between the extremes of full functionality (in which one can do everything, but it is hard to do anything in particular) and naive simplicity (in which it is easy to do the obvious things, but one can't do anything interesting). Minimal buy-in acknowledges that design decisions must be made up-front in order to achieve this balance. Reported here are recent efforts to explore minimal buy-in software through the implementation of Funtools, a small suite of FITS library routines and analysis programs that attempts to hide the complexity of FITS coding. In particular, the use of "natural order" in the Funtools design enables it to "do the right thing" automatically. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Mandel, E (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 0 TC 7 Z9 7 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 225 EP 228 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400049 ER PT B AU Subramanian, S Plummer, D AF Subramanian, S Plummer, D BE Harnden, FR Primini, FA Payne, HE TI The Chandra automatic processing/archive interface SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB The Chandra Automatic Data Processing System (AP) requires quick access to previously generated data. Potential inefficiencies are avoided by introducing a layer between the pipelines and the archive. This archive interface layer includes an archive request queue, a data archiving server (darch), and an archive "cache". The design and functional operation of each of these components are presented in this paper. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Subramanian, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-81, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 303 EP 305 PG 3 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400067 ER PT B AU Doe, S Noble, M Smith, R AF Doe, S Noble, M Smith, R BE Harnden, FR Primini, FA Payne, HE TI Interactive analysis and scripting in CIAO 2.0 SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB Interpreted scripting languages are now recognized as essential components in the programmer's (and user's) tool chest, and, as amply demonstrated at ADASS 1999, have infiltrated the scientific community with great effect. In this paper we discuss the utilization of the S-Lang interpreted language within the Chandra Data Analysis System (CIAO, or Chandra Interactive Analysis of Observations). In only a few months, with substantial reuse and comparatively little manpower and code bloat, this effort has increased by an order of magnitude the analytical power and extensibility of CIAO. We summarize our design and implementation, and show brief fitting, modeling, and visualization threads that demonstrate capabilities roughly comparable with those of commercial packages. Finally, we present a beta version of the CIAO spectroscopic analysis module, GUIDE - largely a collection of S-Lang scripts, glued with C++ enhancements to Sherpa and ChIPS - to illustrate in more depth the range of new functionality and the rapid prototyping now available in CIAO. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Doe, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 81, Cambridge, MA 02138 USA. NR 0 TC 4 Z9 4 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 310 EP 313 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400069 ER PT B AU Demleitner, M Accomazzi, A Eichhorn, G Grant, CS Kurtz, MJ Murray, SS AF Demleitner, M Accomazzi, A Eichhorn, G Grant, CS Kurtz, MJ Murray, SS BE Harnden, FR Primini, FA Payne, HE TI ADS's Dexter Data Extraction Applet SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB The NASA Astrophysics Data System (ADS) now holds 1.3 million scanned pages, containing numerous plots and figures for which the original data sets are lost or inaccessible. The availability of scans of the figures can significantly ease the regeneration of the data sets. For this purpose, the ADS has developed Dexter, a Java applet that supports the user in this process. Dexter's basic functionality is to let the user manually digitize a plot by marking points and defining the coordinate transformation from the logical to the physical coordinate system. Advanced features include automatic identification of axes, tracing lines and finding points matching a template. This contribution both describes the operation of Dexter from a user's point of view and discusses some of the architectural issues we faced during implementation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Demleitner, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Eichhorn, Guenther/C-9480-2009; KURTZ, Michael /B-3890-2009 OI Eichhorn, Guenther/0000-0002-3032-1978; NR 0 TC 26 Z9 26 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 321 EP 324 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400072 ER PT B AU Barth, AJ AF Barth, AJ BE Harnden, FR Primini, FA Payne, HE TI ATV: An image-display tool for IDL SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB The IDL language offers a powerful environment for reduction and analysis of astronomical data. While there are numerous libraries of publicly available IDL routines, one major drawback has been the lack of an image-display program optimized for viewing astronomical images. ATV is a display program written entirely in IDL and designed to emulate the SAOimage and DS9 programs. It works equally well under the Unix, Linux, Windows, and MacOS versions of IDL, and includes features such as interactive control of color stretch, zoom, and image scaling; image blinking; and creation of publication-quality PostScript output. It also includes a simple photometry package suitable for quick-look reductions. The program is freely available via the Internet. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barth, AJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 18 Z9 18 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 385 EP 387 PG 3 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400085 ER PT B AU Adams-Wolk, NR AF Adams-Wolk, NR BE Harnden, FR Primini, FA Payne, HE TI A flexible object oriented design for page formating SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB The Chandra standard data processing now includes a group of summary pages that offer a synopsis of the observation. Chandra's instrument and grating combinations form many different spacecraft configurations. For each configuration, a specific summary of the observation is required. We need a flexible and expandable page formatter to handle this situation. One result of this development is the sum-format-page tool. This C++ tool is built on object oriented design principles and constrain the flexibility to produce multiple output file formats. Here we discuss the motivations for the tool, the design and implementation, and future enhancements that need to be considered. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Adams-Wolk, NR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 419 EP 422 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400094 ER PT B AU Karovska, M Beikman, SJ Elvis, MS Flanagan, JM Gaetz, T Glotfelty, KJ Jerius, D McDowell, JC Rots, AH AF Karovska, M Beikman, SJ Elvis, MS Flanagan, JM Gaetz, T Glotfelty, KJ Jerius, D McDowell, JC Rots, AH BE Harnden, FR Primini, FA Payne, HE TI The Chandra X-Ray Observatory PSF library SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB Pre-flight and on-orbit calibration of the Chandra X-Ray Observatory provided a unique base for developing detailed models of the optics and detectors. Using these models we have produced a set of simulations of the Chandra point spread function (PSF) which is available to the users via PSF library files. We describe here how the PSF models are generated and the design and content of the Chandra PSF library files. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Karovska, M (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. NR 0 TC 5 Z9 5 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 435 EP 438 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400098 ER PT B AU Cresitello-Dittmar, M Aldcroft, TL Morris, D AF Cresitello-Dittmar, M Aldcroft, TL Morris, D BE Harnden, FR Primini, FA Payne, HE TI On the fly bad pixel detection for the Chandra X-Ray Observatory's aspect camera SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB The Chandra X-ray Observatory uses an optical CCD in its aspect camera. As with all space-based CCD detectors, radiation damage will accrue with time and substantially increase the dark current of individual pixels, resulting in "warm pixels." In order to obtain the most accurate aspect solution possible, it is necessary to identify and compensate for these regions when processing the guide star images. If a warm pixel is included in a guide star image, it will bias the centroid location for that image. As the spacecraft dithers, this bias will introduce a wobble to the star location that translates to a wobble in the aspect solution. Special dark current calibration observations can be taken to provide a full-frame dark current map, however, it is not operationally feasible to obtain a new map for each observation. The CXC data systems group has developed software to analyze the star image data and identify warm pixels as part of standard processing. This "on the fly" determination allows us to adjust for variations in CCD conditions between dark current calibration observations and provides useful information for identifying bad regions on the Aspect camera CCD. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cresitello-Dittmar, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 439 EP 442 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400099 ER PT B AU Calderwood, T Dobrzycki, A Jessop, H Harris, DE AF Calderwood, T Dobrzycki, A Jessop, H Harris, DE BE Harnden, FR Primini, FA Payne, HE TI The sliding-cell detection program for Chandra X-Ray data SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB The Chandra X-ray Observatory provides unprecedented resolution over a large field of view with large collecting area. With these advancements, different and/or improved detection algorithms are a necessity for Chandra data analysis. We here present an overview of Celldetect, a source detection program for Chandra. Celldetect is descendent from Einstein and ROSAT data analysis programs (Harnden et al. 1984; DePonte & Primini 1993). It is part of the Chandra Interactive Analysis of Observations (CIAO) software package and is also used in automated processing of Chandra data. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Calderwood, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 5 Z9 5 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 443 EP 446 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400100 ER PT B AU Petreshock, JG Wolk, SJ Cresitello-Dittmar, M Isobe, T AF Petreshock, JG Wolk, SJ Cresitello-Dittmar, M Isobe, T BE Harnden, FR Primini, FA Payne, HE TI An object oriented design for monitoring the Chandra science instrument X-ray background SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB The Monitoring and Trends Analysis (M&TA) System for the Chandra X-ray Observatory consists of multiple software threads designed to monitor and visualize spacecraft behavior. The Science Instrument (SI) background monitoring is one such thread that is designed to compile a temporally and spatially ordered table of the observed flux and energy spectrum in detector coordinates. In this paper we describe the design of the tools, and applications of the data products generated, and the output product flexibility. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Petreshock, JG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 467 EP 470 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400106 ER PT B AU Hain, R Aldcroft, TL Cameron, RA Cresitello-Dittmar, M Karovska, M AF Hain, R Aldcroft, TL Cameron, RA Cresitello-Dittmar, M Karovska, M BE Harnden, FR Primini, FA Payne, HE TI Kalman filtering in Chandra aspect determination SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO ID INITIAL PERFORMANCE AB The ability of the Chandra X-ray Observatory to achieve unprecedented image resolution is due, in part, to its ability to accurately reconstruct the spacecraft attitude history. This is done with a Kalman filter and Rauch-Tung-Striebel (RTS) smoother, which are key components of the overall aspect solution software. The Kalman filter/RTS smoother work by combining data from star position measurements, which are accurate over the long term but individually noisy, and spacecraft rate information from on-board gyroscopes, which are very accurate over the short-term, but are subject to drifts in the bias rate over longer time scales. The strengths of these two measurement sources are complementary. The gyro rate data minimizes the effects of noise from the star measurements, and the long-term accuracy of the star data provides a high-fidelity estimate of the gyro bias drift. Analysis of flight data, through comparison of observed guide star position with expected position and examination of the reconstructed X-ray image point spread function, supports the conclusion that performance goals (1.0 arcsecond mean aspect error, 0.5 arcsecond aspect error spread diameter) were met. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hain, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 471 EP 474 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400107 ER PT B AU Plummer, D Subramanian, S AF Plummer, D Subramanian, S BE Harnden, FR Primini, FA Payne, HE TI The Chandra automatic data processing infrastructure SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB The requirements for processing Chandra telemetry are very involved and complex. To maximize efficiency, the infrastructure for processing telemetry has been automated such that all stages of processing will be initiated without operator intervention once a telemetry file is sent to the processing input directory. To maximize flexibility, the processing infrastructure is configured via an ASCII registry. This paper discusses the major components of the Automatic Processing infrastructure including our use of the STRcI OPUS system. It describes how the registry is used to control and coordinate the automatic processing. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Plummer, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-81, Cambridge, MA 02138 USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 475 EP 478 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400108 ER PT B AU Rots, AH McDowell, JC He, XH Freeman, PE AF Rots, AH McDowell, JC He, XH Freeman, PE BE Harnden, FR Primini, FA Payne, HE TI The FITS embedded function format SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB We have developed a format convention that allows one to specify an n-dimensional function in a FITS binary table, the FITS Embedded Function (FEF). The format allows for enumerated values, constants, and analytical functions, and arithmetic combinations of those three. The parameters of the analytical functions may, again, be enumerated, constant, or function values. The concept is intended to allow the user to extract a multi-dimensional subimage from a FEF in the same way one would extract a subimage from a primary array or image extension. The format is extremely versatile and has many potential applications. Developing a generic FEF extractor is very challenging but will allow very cost-effective reuse. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rots, AH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 81, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 479 EP 482 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400109 ER PT B AU Freeman, PE Doe, S Siemiginowska, A AF Freeman, PE Doe, S Siemiginowska, A BE Harnden, FR Primini, FA Payne, HE TI New elements of sherpa, CIAO's modeling and fitting tool SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB We describe enhancements made to Sherpa for the CIAO 2.0 release, concentrating upon those that enable a user to: (1) analyze Chandra X-ray Observatory grating data with wavelength- or energy-space models; (2) simultaneously fit background and source datasets; and (3) estimate and visualize confidence intervals and regions. We also list enhancements that we plan to make to Sherpa for future CIAO releases. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Freeman, PE (reprint author), Harvard Smithsonian Ctr Astrophys, MS-81,60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 483 EP 486 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400110 ER PT B AU Mink, DJ Kurtz, MJ AF Mink, DJ Kurtz, MJ BE Harnden, FR Primini, FA Payne, HE TI SVDFIT: An IRAF task for eigenvector sky subtraction SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB A new method has been developed for estimating and removing the spectrum of the sky from deep spectroscopic observations. This method does not rely on simultaneous measurement of the sky spectrum with the object spectrum. The technique is based on the iterative subtraction of continuum estimates and eigenvector sky models derived from singular value decompositions of sky spectra and sky spectra residuals. IRAF tasks have been developed to implement this technique. Using simulated data derived from small-telescope observations, we demonstrate that the method is effective for faint objects on large telescopes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mink, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI KURTZ, Michael /B-3890-2009 NR 2 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 491 EP 494 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400112 ER PT B AU He, XH Wise, M Glotfelty, KJ AF He, XH Wise, M Glotfelty, KJ BE Harnden, FR Primini, FA Payne, HE TI Enhancements of MKRMF SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS X SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 10th Annual Conference for Astronomical Data Analysis Software and Systems (ADASS 2000) CY NOV 12-15, 2000 CL BOSTON, MA SP Akibia Inc, Canada France Hawaii Telescope, NASA, Space Telescope Sci Inst, Smithsonian Astrophys Observ, NOAO AB MKRMF, a data analysis tool of the Chandra X-ray Science Center (CXC), has evolved to more effectively create response matrix files (RMF). It provides new and enhanced features: uniform binning syntax, all-inclusive FITS embedded function (FEF) file extraction, and non-linear EBOUNDS calculation. This paper describes the algorithm, application interfaces and highlights of the future development. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP He, XH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-075-7 J9 ASTR SOC P PY 2001 VL 238 BP 518 EP 521 PG 4 WC Astronomy & Astrophysics; Computer Science, Software Engineering SC Astronomy & Astrophysics; Computer Science GA BU31S UT WOS:000175678400119 ER PT J AU Kannappan, SJ Fabricant, DG AF Kannappan, SJ Fabricant, DG TI A broad search for counterrotating gas and stars: Evidence for mergers and accretion SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : formation; galaxies : interactions; galaxies : kinematics and dynamics ID POLAR-RING GALAXIES; ELLIPTIC GALAXIES; DISKS; KINEMATICS; CLUSTER; ORIGIN AB We measure the frequency of bulk gas-stellar counterrotation in a sample of 67 galaxies drawn from the Nearby Field Galaxy Survey, a broadly representative survey of the local galaxy population down to M-B similar to -15. We detect four counterrotators among 17 E/S0's with extended gas emission In (24(-6)(+8)%). contrast, we find no clear examples of bulk counterrotation among 38 Sa-Sbc spirals, although one Sa does show peculiar gas kinematics. This result implies that, at 95% confidence, no more than 8% of Sa-Sbc spirals are bulk counterrotators. Among types Sc and later, we identify only one possible counterrotator, a Magellanic irregular. We use these results together with the physical properties of the counterrotators to constrain possible origins for this phenomenon. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kannappan, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, Mail Stop 20,60 Garden St, Cambridge, MA 02138 USA. NR 45 TC 45 Z9 45 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2001 VL 121 IS 1 BP 140 EP 147 DI 10.1086/318027 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 388GY UT WOS:000166173300011 ER PT J AU Kenyon, SJ Bromley, BC AF Kenyon, SJ Bromley, BC TI Gravitational stirring in planetary debris disks SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; solar system : formation; stars : formation ID MAIN-SEQUENCE STARS; VEGA-TYPE SYSTEMS; EARLY KUIPER-BELT; CIRCUMSTELLAR DISK; BETA-PICTORIS; SOLAR-SYSTEM; ACCRETIONAL EVOLUTION; PLANETESIMAL SWARM; RUNAWAY GROWTH; TIME SCALES AB We describe gravitational stirring models of planetary debris disks using a new multiannulus planetesimal evolution code. The current code includes gravitational stirring and dynamical friction; future studies will include coagulation, fragmentation, Poynting-Robertson drag, and other physical processes. We use the results of our calculations to investigate the physical conditions required for small bodies in a planetesimal disk to reach the shattering velocity and begin a collisional cascade. Our results demonstrate that disks composed primarily of bodies with a single size will not undergo a collisional cascade that produces small dust grains at 30-150 AU on timescales of 1 Gyr or smaller. Disks with a size distribution of bodies reach conditions necessary for a collisional cascade in 10 Myr to 1 Gyr if the disk is at least as massive as a minimum mass solar nebula and if the disk contains objects with radii of 500 km or larger. The estimated similar to 500 Myr survival time for these disks is close to the median age of similar to 400 Myr derived for nearby stars with dusty disks. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 61 TC 69 Z9 69 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2001 VL 121 IS 1 BP 538 EP 551 DI 10.1086/318019 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 388GY UT WOS:000166173300045 ER PT J AU Comastri, A Stirpe, GM Vignali, C Brandt, WN Leighly, KM Fiore, F Guainazzi, M Matt, G Nicastro, F Puchnarewicz, EM Siemiginowska, A AF Comastri, A Stirpe, GM Vignali, C Brandt, WN Leighly, KM Fiore, F Guainazzi, M Matt, G Nicastro, F Puchnarewicz, EM Siemiginowska, A TI BeppoSAX observations of Narrow-Line Seyfert 1 galaxies - II. Ionized iron features in Arakelian 564 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays : galaxies; galaxies : Seyfert; galaxies : individual : Ark 564 ID X-RAY ASTRONOMY; ENERGY CONCENTRATOR SPECTROMETER; ON-BOARD; ACCRETION DISKS; VARIABILITY; SATELLITE; REFLECTION; SPECTRA; ASCA AB The BeppoSAX observations of the bright Narrow-Line Seyfert I galaxy Ark 564 are presented along with a high quality optical spectrum taken at the 1.5 m telescope at La Silla. The 0.1-10 keV X-ray spectrum is characterized by a strong soft; component which is best described by blackbody-like emission with a temperature of similar to 160 eV. At higher energies a steep (Gamma similar or equal to 2.4) power-law tail is present. There is evidence of an ionized reflector in the form of an iron line and edge. We do not find significant evidence of soft X-ray features if the spectrum is modelled with a two component continuum. The optical and X-ray spectral properties support the hypothesis of a high accretion rate onto a low mass black hole. C1 Osservatorio Astron Bologna, I-40127 Bologna, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. Columbia Univ, Dept Astron, New York, NY 10027 USA. Osserv Astron Roma, I-00044 Monte Porzio Catone, Italy. SAX, Sci Data Ctr, Nuova Telespazio, I-00131 Rome, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. ESA, VILSPA, XMM Newton SOC, E-28080 Madrid, Spain. Univ Roma Tre, Dipartimetno Fis E Amaldi, I-00146 Rome, Italy. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy. EM comastri@bo.astro.it RI Vignali, Cristian/J-4974-2012; Brandt, William/N-2844-2015; Stirpe, Giovanna/O-9393-2015; Comastri, Andrea/O-9543-2015; OI Vignali, Cristian/0000-0002-8853-9611; Brandt, William/0000-0002-0167-2453; Stirpe, Giovanna/0000-0002-3702-8731; Comastri, Andrea/0000-0003-3451-9970; Nicastro, Fabrizio/0000-0002-6896-1364; Fiore, Fabrizio/0000-0002-4031-4157 NR 32 TC 28 Z9 28 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2001 VL 365 IS 3 BP 400 EP 408 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 402PV UT WOS:000166998100006 ER PT J AU Meeus, G Waters, LBFM Bouwman, J van den Ancker, ME Waelkens, C Malfait, K AF Meeus, G Waters, LBFM Bouwman, J van den Ancker, ME Waelkens, C Malfait, K TI ISO spectroscopy of circumstellar dust in 14 Herbig Ae/Be systems: Towards an understanding of dust processing SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE circumstellar matter; stars : pre-main sequence; infrared : ISM : lines and bands; solar system : formation ID SPECTRAL ENERGY-DISTRIBUTIONS; T-TAURI STARS; SWS OBSERVATIONS; ACCRETION DISKS; HIGH-RESOLUTION; LIMITS; GRAINS; SHELL AB We present Infrared Space Observatory (ISO) spectra of fourteen isolated Herbig; Ae/Be (HAEBE) stars, to study the characteristics of their circumstellar dust. These spectra show large star-to-star differences, in the emission features of both carbon-rich and oxygen-rich dust grains. The IR spectra were combined with photometric data ranging from the UV through the optical into the sub-mm region. We defined two key groups, based upon the spectral shape of the infrared region. The derived results can be summarized as follows: (1) the continuum of the IR to sub-mm region of all stars can be reconstructed by the sum of a power-law and a cool component, which can be represented by a black body. Possible locations for these components are an optically thick, geometrically thin disc (power-law component) and an optically thin hared region (black body); (2) all stars have a substantial amount of cold dust around them, independent of the amount of mid-IR excess they show; (3) also the near-IR excess is unrelated to the mid-IR excess, indicating different composition/location of the emitting material; (4) remarkably, some sources lack the silicate bands; (5) apart from amorphous silicates, we find evidence for crystalline silicates in several stars, some of which are new detections; (6) PAH bands are present in at least 50% of our sample, and their appearance is slightly different from PAHs in the ISM; (7) PAH bands are, with one exception, not present in sources which only show a power-law continuum in the IR; their presence is unrelated to the presence of the silicate bands; (8) the dust in HAEBE stars shows strong evidence for coagulation; this dust processing is unrelated to any of the central star properties (such as age, spectral type and activity). C1 Katholieke Univ Leuven, Astron Inst, B-3001 Heverlee, Belgium. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Meeus, G (reprint author), Katholieke Univ Leuven, Astron Inst, Celestijnenlaan 200B, B-3001 Heverlee, Belgium. EM gwendolyn@ster.kuleuven.ac.be NR 49 TC 394 Z9 396 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2001 VL 365 IS 3 BP 476 EP 490 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 402PV UT WOS:000166998100013 ER PT J AU Wolf, C Meisenheimer, K Roser, HJ Beckwith, SVW Chaffee, FH Fried, J Hippelein, H Huang, JS Kummel, M von Kuhlmann, B Maier, C Phleps, S Rix, HW Thommes, E Thompson, D AF Wolf, C Meisenheimer, K Roser, HJ Beckwith, SVW Chaffee, FH Fried, J Hippelein, H Huang, JS Kummel, M von Kuhlmann, B Maier, C Phleps, S Rix, HW Thommes, E Thompson, D TI Multi-color classification in the calar alto deep imaging survey SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods : data analysis; methods : statistical; techniques : photometric; surveys ID LUMINOSITY FUNCTION; QUASARS; GALAXIES; COUNTS AB We use a multi-color classification method introduced by Wolf et al. (2001) to reliably identify stars, galaxies and quasars in the up to 16-dimensional color space: provided by the filter set of the Calar Alto Deep Imaging Survey (CADIS). The samples of stars, galaxies and quasars obtained this way have been used for dedicated studies which are published in separate papers. The classification is good enough to detect quasars rather completely and efficiently without confirmative spectroscopy. The multi-color redshifts are accurate enough for most statistical applications, e.g. evolutionary studies of the galaxy luminosity function. Also, the separation between stars and galaxies reaches deeper than with morphological criteria, so that studies of the stellar population can be extended to fainter levels. We characterize the dataset presently available on the CADIS 1 h-, 9 h- and 16 h-fields. Using Monte-Carlo simulations we model the classification performance expected for CADIS. We present a summary of the classification results on the CADIS database and discuss unclassified objects. More than 99% of the whole catalog sample at R < 22 (more than 95% at R < 23) are successfully classified matching the expectations derived from the simulations. A small number of peculiar objects challenging the classification is discussed in detail. Spectroscopic observations are used to check the reliability of the multi-color classification (6 mistakes among 151 objects with R < 24). From these, we also determine the accuracy of the multi-color redshifts which are rather good for galaxies ((z) approximate to 0.03) and useful for quasars. We find that the classification performance derived from the simulations compares well with results from the real survey. Finally, we locate areas for potential improvement of the classification. C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany. Space Telescope Sci Inst, Baltimore, MD 21218 USA. WM Keck Observ, Kamuela, HI 96743 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Pasadena, CA 91125 USA. RP Wolf, C (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM cwolf@mpia-hd.mpg.de OI Maier, Christian/0000-0001-6405-2182 NR 29 TC 46 Z9 46 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2001 VL 365 IS 3 BP 681 EP 698 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 402PV UT WOS:000166998100031 ER PT J AU Watson, MG Augueres, JL Ballet, J Barcons, X Barret, D Boer, M Boller, T Bromage, GE Brunner, H Carrera, FJ Cropper, MS Denby, M Ehle, M Elvis, M Fabian, AC Freyberg, MJ Guillout, P Hameury, JM Hasinger, G Hinshaw, DA Maccacaro, T Mason, KO McMahon, RG Michel, L Mirioni, L Mittaz, JP Motch, C Olive, JF Osborne, JP Page, CG Pakull, M Perry, BH Pierre, M Pietsch, W Pye, JP Read, AM Roberts, TP Rosen, SR Sauvageot, JL Schwope, AD Sekiguchi, K Stewart, GC Stewart, I Valtchanov, I Ward, MJ Warwick, RS West, RG White, NE Worrall, DM AF Watson, MG Augueres, JL Ballet, J Barcons, X Barret, D Boer, M Boller, T Bromage, GE Brunner, H Carrera, FJ Cropper, MS Denby, M Ehle, M Elvis, M Fabian, AC Freyberg, MJ Guillout, P Hameury, JM Hasinger, G Hinshaw, DA Maccacaro, T Mason, KO McMahon, RG Michel, L Mirioni, L Mittaz, JP Motch, C Olive, JF Osborne, JP Page, CG Pakull, M Perry, BH Pierre, M Pietsch, W Pye, JP Read, AM Roberts, TP Rosen, SR Sauvageot, JL Schwope, AD Sekiguchi, K Stewart, GC Stewart, I Valtchanov, I Ward, MJ Warwick, RS West, RG White, NE Worrall, DM TI The XMM-Newton serendipitous survey I. The role of XMM-Newton Survey Science Centre SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE surveys; methods : data analysis; X-rays : general; X-rays : galaxies; X-rays : stars ID MEDIUM-SENSITIVITY SURVEY; PHOTON IMAGING CAMERA; ROSAT DEEP SURVEY; X-RAY SOURCES; LOCKMAN-HOLE AB This paper describes the performance of XMM-Newton for serendipitous surveys and summarises the scope and potential of the XMM-Newton Serendipitous Survey. The role of the Survey Science Centre (SSC) in the XMM-Newton project is outlined. The SSC's follow-up and identification programme for the XMM-Newton serendipitous survey is described together with the presentation of some of the first results. C1 Univ Leicester, Dept Phys & Astron, Xray AStron Grp, Leicester LE1 7RH, Leics, England. CEA Saclay, DSM, DAPNIA, SAp, F-91191 Gif Sur Yvette, France. UC, CSIC, Inst Fis Cantabria, Santander 39005, Spain. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Observ Astron, F-67000 Strasbourg, France. Osserv Astron Brera, I-20121 Milan, Italy. Subaru Telescope, NAOJ, Hilo, HI 96720 USA. NASA, Goddard Space Flight Ctr, LHEA, Greenbelt, MD 20771 USA. Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. XMM Newton SOC, Madrid 28080, Spain. RP Univ Leicester, Dept Phys & Astron, Xray AStron Grp, Leicester LE1 7RH, Leics, England. RI White, Nicholas/B-6428-2012; Barcons, Xavier/L-3335-2014; OI White, Nicholas/0000-0003-3853-3462; Barcons, Xavier/0000-0003-1081-8861; McMahon, Richard/0000-0001-8447-8869; Hameury, Jean-Marie/0000-0002-6412-0103; Boer, Michel/0000-0001-9157-4349 NR 13 TC 94 Z9 94 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JAN PY 2001 VL 365 IS 1 BP L51 EP L59 DI 10.1051/0004-6361:20000067 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 392RV UT WOS:000166426300008 ER PT J AU Barth, AJ Ho, LC Filippenko, AV Rix, HW Sargent, WLW AF Barth, AJ Ho, LC Filippenko, AV Rix, HW Sargent, WLW TI The broad-line and narrow-line regions of the liner NGC 4579 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 4579); galaxies : nuclei; galaxies : Seyfert ID ACTIVE GALACTIC NUCLEI; PEAKED EMISSION-LINES; DWARF SEYFERT NUCLEI; IRON K-LINE; BLACK-HOLE; NGC 4579; ACCRETION DISK; ULTRAVIOLET-SPECTRUM; SPIRAL GALAXIES; HOST GALAXIES AB We report the discovery of an extremely broad H alpha emission line in the LINER nucleus of NGC 4579. From ground-based observations, the galaxy was previously known to contain a type 1 nucleus with a broad H alpha line of FWHM approximate to 2300 km s(-1) and FWZI approximate to 5000 km s(-1). New spectra obtained with the Hubble Space Telescope (HST) and a 0.2" wide slit reveal an H alpha component with an FWZI of similar to 18,000 km s(-1). The line is not obviously double peaked, but it does possess "shoulders" on the red and blue sides which resemble the profiles seen in double-peaked emitters such as NGC 4203 and NGC 4450. This similarity suggests that the very broad H alpha profile in NGC 4579 may represent emission from an accretion disk. Three such objects have been found recently in two HST programs which have targeted a total of 30 galaxies, demonstrating that double-peaked or extremely broad-line emission in LINERs must be much more common than would be inferred from ground-based surveys. The ratio of the narrow [S II] lambda lambda 6716, 6731 lines shows a pronounced gradient indicating a steep rise in density toward the nucleus. The direct detection of a density gradient within the inner arcsecond of the narrow-line region confirms expectations from previous observations of line width-critical density correlations in several LINERs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. CALTECH 105 24, Palomar Observ, Pasadena, CA 91125 USA. RP Barth, AJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 44 TC 59 Z9 60 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2001 VL 546 IS 1 BP 205 EP 209 DI 10.1086/318268 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 390DL UT WOS:000166280400017 ER PT J AU Paerels, F Brinkman, AC van der Meer, RLJ Kaastra, JS Kuulkers, E den Boggende, AJF Predehl, P Drake, JJ Kahn, SM Savin, DW McLaughlin, BM AF Paerels, F Brinkman, AC van der Meer, RLJ Kaastra, JS Kuulkers, E den Boggende, AJF Predehl, P Drake, JJ Kahn, SM Savin, DW McLaughlin, BM TI Interstellar X-ray absorption spectroscopy of oxygen, neon, and iron with the Chandra LETGS spectrum of X0614+091 SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; ISM : general; stars : individual (X0614+091); techniques : spectroscopic; X-rays : stars ID TRANSMISSION GRATING SPECTROMETER; CROSS-SECTIONS; ATOMIC OXYGEN; K-EDGE; AXAF; RESOLUTION; PHOTOABSORPTION; CALIBRATION; IONIZATION; SCATTERING AB We find resolved interstellar O K, Ne K, and Fe L absorption spectra in the Chandra X-Ray Observatory Low-Energy Transmission Grating Spectrometer (LETGS) spectrum of the low-mass X-ray binary X0614+091. We measure the column densities in O and Ne and find direct spectroscopic constraints on the chemical state of the interstellar O. These measurements probably probe a low-density line of sight through the Galaxy, and we discuss the results in the context of our knowledge of the properties of interstellar matter in regions between the spiral arms. C1 Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. SRON, Space Res Lab, NL-3584 CA Utrecht, Netherlands. Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Queens Univ Belfast, Dept Appl Math & Theoret Phys, Belfast BT7 1NN, Antrim, North Ireland. Univ Utrecht, Inst Astron, NL-3507 TA Utrecht, Netherlands. RP Paerels, F (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. RI Savin, Daniel/B-9576-2012 OI Savin, Daniel/0000-0002-1111-6610 NR 30 TC 84 Z9 84 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2001 VL 546 IS 1 BP 338 EP 344 DI 10.1086/318251 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 390DL UT WOS:000166280400030 ER PT J AU Song, I Caillault, JP Navascues, DBY Stauffer, JR AF Song, I Caillault, JP Navascues, DBY Stauffer, JR TI Ages of A-type Vega-like stars from uvby beta photometry SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared : stars; planetary systems; stars : early-type ID BROWN DWARF CANDIDATES; MAIN-SEQUENCE STARS; EFFECTIVE TEMPERATURE; PRECISE DETERMINATION; SURFACE GRAVITY; KECK SPECTRA; B-STAR; F-STAR; FOMALHAUT; ROTATION AB We have estimated the ages of a sample of A-type Vega-like stars by using Stromgren uvby beta photometric data and theoretical evolutionary tracks. We find that 13% of these A stars have been reported as Vega-like stars in the literature and that the ages of this subset run the gamut from very young (50 Myr) to old (1 Gyr), with no obvious age difference compared to those of field A stars. We clearly show that the fractional IR luminosity decreases with the ages of Vega-like stars. C1 Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Song, I (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. RI Barrado Navascues, David/C-1439-2017 OI Barrado Navascues, David/0000-0002-5971-9242 NR 36 TC 78 Z9 78 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2001 VL 546 IS 1 BP 352 EP 357 DI 10.1086/318269 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 390DL UT WOS:000166280400032 ER PT J AU Millan-Gabet, R Schloerb, FP Traub, WA AF Millan-Gabet, R Schloerb, FP Traub, WA TI Spatially resolved circumstellar structure of herbig Ae/Be stars in the near-infrared SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; circumstellar matter; infrared : stars; instrumentation : interferometers; stars : formation; techniques : interferometric ID INTERMEDIATE-MASS STARS; IOTA INTERFEROMETER; FORBIDDEN LINES; ACCRETION DISKS; EVOLUTION; EMISSION; AE; DIAGNOSTICS; EXTINCTION; ENVELOPES AB We have conducted the first systematic study of Herbig Ae/Be stars using the technique of long baseline stellar interferometry in the near-infrared, with the objective of characterizing the distribution and properties of the circumstellar dust responsible for the excess near-infrared fluxes from these systems. The observations for this work have been conducted at the Infrared Optical Telescope Array (IOTA). The principal result of this paper is that the interferometer resolves the source of infrared excess in 11 of the 15 systems surveyed. A new binary, MWC 361-A, has been detected interferometrically for the first time. The visibility data for all the sources has been interpreted within the context of four simple models which represent a range of plausible representations for the brightness distribution of the source of excess emission: a Gaussian, a narrow uniform ring, a flat blackbody disk with a single temperature power law, and an infrared companion. We find that the characteristic sizes of the near-infrared emitting regions are larger than previously thought (0.5-5.9 AU, as given by the FWHM of the Gaussian intensity). A further major result of this paper is that the sizes measured, when combined with the observed spectral energy distributions, essentially rule out accretion disk models represented by black-body disks with the canonical T (r) proportional to r(-3/4) law. We also find that, within the range observed in this study, none of the sources (except the new binary) shows varying visibilities as the orientation of the interferometer baseline changes. This is the expected behavior for sources which appear circularly symmetric on the sky, and for the sources with the largest baseline position angle coverage (AB Aur, MWC 1080-A) asymmetric brightness distributions (such as inclined disks or binaries) become highly unlikely. Taken as an ensemble, with no clear evidence in favor of axisymmetric structure, the observations favor the interpretation that the circumstellar dust is distributed in spherical envelopes (the Gaussian model) or thin shells (the ring model). This interpretation is also supported by the result that the measured sizes, combined with the excess near-infrared fluxes, imply emission of finite optical depth, as required by the fact that the central stars are optically visible. The measured sizes and brightnesses do not correlate strongly with the luminosity of the central star. Moreover, in two cases, the same excess is observed from circumstellar structures that differ in size by more than a factor of 2 and surround essentially identical stars. Therefore, different physical mechanisms for the near-infrared emission may be at work in different cases, or alternatively, a single underlying mechanism with the property that the same infrared excess is produced on very different physical scales. C1 Univ Massachusetts, Dept Phys & Astron, Amherst, MA 01003 USA. RP Millan-Gabet, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 41 TC 167 Z9 169 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2001 VL 546 IS 1 BP 358 EP 381 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 390DL UT WOS:000166280400033 ER PT J AU Ransom, SM Greenhill, LJ Herrnstein, JR Manchester, RN Camilo, F Eikenberry, SS Lyne, AG AF Ransom, SM Greenhill, LJ Herrnstein, JR Manchester, RN Camilo, F Eikenberry, SS Lyne, AG TI A binary millisecond pulsar in globular cluster NGC 6544 SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters : individual (NGC 6544); pulsars : individual (PSR J1807-2459) radio continuum : stars ID X-RAY BINARIES; RADIO PULSARS; SUPERNOVA-REMNANTS; DISCOVERY; SEARCH AB We report the detection of a new 3.06 ms binary pulsar in the globular cluster NGC 6544 using a Fourier-domain "acceleration" search. With an implied companion mass of similar to0.01 M. and an orbital period of only P-b similar to 1.7 hr, it displays orbital properties very similar to many pulsars that are eclipsed by their companion winds. The orbital period is the second shortest of known binary pulsars after 47 Tuc R. The measured flux density of 1.3 +/- 0.4 mJy at 1332 MHz indicates that the pulsar is almost certainly the known steep-spectrum point source near the core of NGC 6544. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. RP Ransom, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Ransom, Scott/0000-0001-5799-9714 NR 34 TC 20 Z9 21 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2001 VL 546 IS 1 BP L25 EP L28 DI 10.1086/318062 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393EV UT WOS:000166457000006 ER PT J AU Wargelin, BJ Drake, JJ AF Wargelin, BJ Drake, JJ TI Observability of stellar winds from late-type dwarfs via charge exchange x-ray emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; ISM : structure; stars : winds, outflows; X-rays : stars ID EXTREME-ULTRAVIOLET EMISSION; LATE-TYPE STARS; ALL-SKY SURVEY; SOLAR-WIND; MASS-LOSS; LIMITS; COMETS; IONS AB Despite the fact that the overwhelming majority of stars are of late spectral type (F-M) and lie on the main sequence, we know nothing about their stellar winds. Existing measurements of winds only apply to high-mass O and B stars, red giants, and supergiants and only extend down to a few times 10(-10) M. yr(-1), as compared to the solar rate of similar to2 x 10(-14) M. y(r-1). Attempts to detect winds from late-type dwarf stars have to date resulted only in loose upper limits of order 10(-12) to 10(-11) M. yr(-1). We propose a novel method of studying stellar winds through observation of charge exchange-induced X-ray emission. Recent X-ray detections of comets suggest that charge transfer between highly charged ions in the solar wind and neutral gases in cometary atmospheres is responsible for much or all of the observed emission, a hypothesis that has been strengthened by Chandra observations of comet C/1999 S4 (LINEAR). It has also been proposed that charge transfer between the solar wind and the local interstellar medium (ISM) produces a substantial fraction of the soft X-ray background observed by ROSAT and various rocket experiments. We show that the same process may be observable in nearby dwarf star systems using Chandra and future large-area high-resolution observatories, which would provide hitherto unobtainable information on wind geometry, ion composition, mass-loss rates, and the distribution of neutral gas in the ISM. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wargelin, BJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 36 TC 59 Z9 59 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2001 VL 546 IS 1 BP L57 EP L60 DI 10.1086/318066 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393EV UT WOS:000166457000013 ER PT S AU Kalogera, V Belczynski, K AF Kalogera, V Belczynski, K BE Centrella, JM TI Event rates for binary inspiral SO ASTROPHYSICAL SOURCES FOR GROUND-BASED GRAVITATIONAL WAVE DETECTORS SE AIP Conference Proceedings LA English DT Proceedings Paper CT Workshop on Astrophysical Sources for Ground-Based Gravitational Wave Detectors CY OCT 30-NOV 01, 2000 CL DREXEL UNIV, PHILADELPHIA, PA HO DREXEL UNIV ID NEUTRON-STAR BINARIES; PULSAR; COALESCENCE; ACCRETION; EVOLUTION; SYSTEM; GALAXY; MASS AB Double compact objects (neutron stars and black holes) found in binaries with small orbital separations are known to spiral in and are expected to coalesce eventually because of the emission of gravitational waves. Such inspiral and merger events are thought to be primary sources for ground based gravitational-wave interferometric detectors (such as LIGO). Here, we present a brief review of estimates of coalescence rates and we examine the origin and relative importance of uncertainties associated with the rate estimates. For the case of double neutron star systems, we compare the most recent rate estimates to upper limits derived in a number of different ways. We also discuss the implications of the formation of close binaries with two non-recycled pulsars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 30 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0014-8 J9 AIP CONF PROC PY 2001 VL 575 BP 107 EP 118 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS56P UT WOS:000170337900010 ER PT J AU Huchra, J AF Huchra, J TI The evolution of galaxies: Unsolved problems and future prospects SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE galaxies; galaxy evolution ID SPACE-TELESCOPE; UNIVERSE; STATE AB We've had an extremely interesting conference covering the observational aspects of galaxy evolution near and far. We've come a very long way since the earliest papers in the 1960's by Tinsley and others first quantified the photometric evolution of galaxies. In this summary, I will first go over some of the things that we know, such as the background that is often not discussed but which is important to keep in mind while looking at new evidence. These include the great progress that has been made on the cosmological model and the identification of fluctuations in the Cosmic microwave background. I'll follow that with a description of what we have learned at this Granadian Euroconference and the questions that either have been newly raised or have remained to be solved in the future, many of which are not at all new and are decidedly non-trivial to attack. The article finishes with a description of some promises for the future plus some general caveats about the way we do research, including Tarzan's dilemma. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM huchra@cfa.harvard.edu NR 23 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X EI 1572-946X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2001 VL 277 SU 1 BP 621 EP 630 DI 10.1023/A:1012798711694 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 492KQ UT WOS:000172167900163 ER PT J AU Schnopper, HW Silver, E Murray, S Romaine, S Bandler, S Jones, C Forman, W Madden, N Beeman, J Haller, E Christensen, F Westergaard, N Fabregat, J Reglero, V Gimenez, A Brosch, N Liebowitz, E Netzer, H Barbera, M Collura, A Sciortino, S AF Schnopper, HW Silver, E Murray, S Romaine, S Bandler, S Jones, C Forman, W Madden, N Beeman, J Haller, E Christensen, F Westergaard, N Fabregat, J Reglero, V Gimenez, A Brosch, N Liebowitz, E Netzer, H Barbera, M Collura, A Sciortino, S TI XRASE: The X-Ray Spectroscopic Explorer SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article AB The X-Ray Spectroscopic Explorer (XRASE) has a unique combination of features that will make it possible to address many of NASA's scientific goals. These include how galaxy clusters form, the physics and chemistry of the ISM, the heating of stellar coronae, the amount and content of intergalactic baryonic matter, the mass of black holes and the formation of disks and jets in AGN and galactic binaries. XRASE has a thin foil, multilayered telescope with a large collecting area up to 10 keV, especially in the Fe K alpha region (1100 cm(2)). Its microcalorimeter array combines high energy resolution (7 eV at 6 keV) and efficiency with a field-of-view of 26 arcmin(2) . A deep orbit allows for long, continuous observations. Monitoring instruments in the optical (WOM-X), UV (TAUVEX) and hard X-RAY (GRAM) bands will offer exceptional opportunities to make simultaneous multi-wavelength observations. C1 Smithsonian Astrophys Lab, Cambridge, MA 02138 USA. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. Danish Space Res Inst, DK-2100 Copenhagen, Denmark. Univ Valencia, Astron & Space Sci Grp, Edificio Invest, E-46100 Burjassot, Spain. INTA, Lab Astrofis & Fis Fundamental, E-28080 Madrid, Spain. Tel Aviv Univ, Sch Phys & Astron, Wise Observ, IL-69978 Tel Aviv, Israel. Osservatorio Astron Palermo Giuseppe S Vaiana, I-90134 Palermo, Italy. RP Schnopper, HW (reprint author), Smithsonian Astrophys Lab, 60 Garden St, Cambridge, MA 02138 USA. RI Brosch, Noah/C-7889-2009; Bandler, Simon/A-6258-2010; Fabregat, Juan/F-9066-2016; OI Barbera, Marco/0000-0002-3188-7420; Bandler, Simon/0000-0002-5112-8106; Fabregat, Juan/0000-0002-5986-9347; collura, alfonso/0000-0001-9534-1235 NR 7 TC 0 Z9 0 U1 1 U2 2 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2001 VL 276 IS 1 BP 49 EP 65 DI 10.1023/A:1012023012177 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467VV UT WOS:000170725200007 ER PT J AU Merloni, A Di Matteo, T Fabian, AC AF Merloni, A Di Matteo, T Fabian, AC TI XTE J1118+480: Clues on the nature of the accretion flow from the optical variability SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 3rd Microquasar Workshop on Galactic Relativistic Jet Sources CY SEP 11-13, 2000 CL GRANADA, SPAIN SP Inst Astrofis Andaluc, Spainish Consejo Super Invest Cientif, Univ Barcelona, Lab Astrofis Espacial Fis Fdn, Inst Nacl Tecn Aerosp ID RAY AB We show how the simultaneous presence of a strong quasi periodic oscillation (QPO) of period similar to 10 seconds in the optical and X-ray lightcurves of the X-ray transient XTE J1118+480 can be used to obtain information about the nature of the accretion Mow around the source. The unusually high optical-to-X-ray flux ratio and the QPO observed simultaneously in both energy bands suggest that a significant fraction of the optical flux might originate close to the central source, where most of the X-rays are produced and be indicative of a magnetically dominated corona. We also show how the temporal evolution of the QPO can provide us with information on both the inner radius and the viscous properties of the optically thick accretion disc. C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Merloni, A (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. RI Di Matteo, Tiziana/O-4762-2014 OI Di Matteo, Tiziana/0000-0002-6462-5734 NR 12 TC 3 Z9 3 U1 0 U2 1 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2001 VL 276 SU S BP 213 EP 216 DI 10.1023/A:1011668001597 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 481BW UT WOS:000171500900055 ER PT J AU Pahre, MA Djorgovski, SG De Carvalho, RR AF Pahre, MA Djorgovski, SG De Carvalho, RR TI The evolutionary history of early-type galaxies as derived from the fundamental plane SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Euroconference on the Evolution of Galaxies on Cosmological Timescales CY NOV 30-DEC 05, 1998 CL PUERTO CRUZ, SPAIN SP European Union ID COLOR-MAGNITUDE RELATION; ELLIPTICAL GALAXIES; DISTANT CLUSTERS; SPECTROSCOPY; PHOTOMETRY AB The fundamental plane (FP) scaling relations and their evolution are a powerful tool for studying the global properties of early-type galaxies and their evolutionary history. The form of the FP, as derived by surveys in the local Universe at wavelengths ranging from the U to the K band, cannot be explained by metallicity variations alone among early-type galaxies; systematic variations in age, dark matter content, or homology breaking are required. A large-scale study of early-type galaxies at 0.1 < z < 0.6 demonstrates that the SB intercept of the FP, the rest frame (U-V) colour, and the absorption line strengths all evolve passively, thereby implying a high mean formation redshift for the stellar content. The slope of the FP evolves with redshift, which is broadly consistent with systematic age effects occurring along the early-type galaxy sequence. The implication that the least luminous early-type galaxies formed later than the luminous galaxies is discussed in the context of the evolution of the colour-magnitude relation, the Butcher-Oemler effect and hierarchical galaxy formation models. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Palomar Observ, Pasadena, CA 91125 USA. MCT, Observ Nacl, Dept Astrofis, BR-20921030 Sao Cristovao, RJ, Brazil. RP Pahre, MA (reprint author), Harvard Smithsonian Ctr Astrophys, Mail Stop 20,60 Garden St, Cambridge, MA 02138 USA. NR 25 TC 5 Z9 5 U1 0 U2 1 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2001 VL 276 IS 2-4 BP 983 EP 990 DI 10.1023/A:1017528430583 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 471TU UT WOS:000170945400081 ER PT J AU Jansen, RA Kannappan, SJ AF Jansen, RA Kannappan, SJ TI The Nearby Field Galaxy Survey - A spectrophotometric and photometric study of nearby galaxies SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT Euroconference on the Evolution of Galaxies on Cosmological Timescales CY NOV 30-DEC 05, 1998 CL PUERTO CRUZ, SPAIN SP European Union ID SURFACE PHOTOMETRY; CLUSTER AB We report on our observing programme to obtain integrated spectrophotometry, intermediate- and high-resolution major-axis spectra, and U B R surface photometry of a representative sample of similar to 200 galaxies in the nearby field. The main goal of this programme is to provide a comparison sample for high-redshift studies and to study the variation in star formation rates (SFRs), star formation history (SFH), excitation, metallicity, and internal kinematics over a wide range of galaxy luminosities and morphological types. In particular, we extend the work of Kennicutt (1992) to lower-luminosity systems. We present the main results of our analysis so far. In these proceedings, we condense the two atlases presented of 1) images and radial surface brightness profiles and colour profiles, and 2) images and integrated spectra into several example images, profiles and spectra, showing the general trends observed. For the original atlases we refer the reader to the electronic distribution on CDROM or as available on the Web at http://www.astro.rug.nl/similar to nfgs/. C1 Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jansen, RA (reprint author), ESA, Estec, Dept Space Sci, Div Astrophys, Postbus 299, NL-2200 AG Noordwijk, Netherlands. NR 15 TC 7 Z9 7 U1 0 U2 2 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PY 2001 VL 276 IS 2-4 BP 1151 EP 1159 DI 10.1023/A:1011954916413 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 471TU UT WOS:000170945400101 ER PT J AU Hunt, JS Bermingham, E Ricklefs, RE AF Hunt, JS Bermingham, E Ricklefs, RE TI Molecular systematics and biogeography of Antillean thrashers, tremblers, and mockingbirds (Aves : Mimidae) SO AUK LA English DT Article ID MITOCHONDRIAL-DNA; TREE TOPOLOGIES; EVOLUTION; SEQUENCE; MODEL; SUBSTITUTION; VERTEBRATES; WARBLERS; CYCLES; ORDER AB We constructed phylogenetic hypotheses for Greater and Lesser Antillean Mimidae, including five endemic species of tremblers and thrashers that represent the best plausible example of an avian radiation within the Lesser Antilles. Phylogenetic relationships were inferred from analysis of 3,491 base pairs (bp) of mitochondrial DNA (mtDNA) and roughly 780 bp of the nuclear-encoded myoglobin gene. We used a subset of mtDNA gene sequences and pcrRFLP analysis to evaluate the phylogeographic relationships among individuals representing island populations of the Brown and Gray tremblers (Cinclocerthia ruficauda and C. gutturalis), Pearly-eyed Thrasher (Margarops fuscatus), Scaly-breasted Thrasher (Margarops fuscus), and Antillean and continental populations of the Tropical (Mimus gilvus) and Northern mockingbirds (Mimus polyglottos). Phylogeographic analysis distinguished three strongly differentiated mtDNA clades among tremblers, as well as distinct southern (St. Lucia and Martinique) and northern (Dominica to Montserrat) mtDNA lineages of the Scaly-breasted Thrasher. Minor geographic subdivision was also observed between continental and Antillean populations of the Tropical Mockingbird. Phylogenetic analyses of species-level Mimidae relationships that are based on mtDNA and nuclear sequences provide strong support for the monophyly and Antillean origin of a clade that consists of the tremblers, pearly-eyed Thrasher, and Scaly-breasted Thrasher, but reject the monophyly of the genus Margarops. Phylogenetic analysis cannot confirm the monophyly of all endemic Antillean mimids because of the apparently contemporaneous diversification of the Antillean White-breasted Thrasher (Ramphocinclus brachyurus) with the continental Gray Catbird (Dumetella carolinensis) and Black Catbird (Melanoptila glabrirostris). However, an insertion and a deletion in the myoglobin intron 2 sequence support grouping the West Indian thrashers and tremblers, from which eve infer that the endemic Lesser Antillean mimids are an indigenous radiation. Assuming a constant mtDNA clock for the Mimidae the splitting of the Northern and Tropical mockingbird lineages is roughly contemporaneous with the separation of the three trembler clades, as well as the two Scaly-breasted Thrasher clades. Application of a mitochondrial DNA dock ticking at 2% sequence divergence per million years (Ma), suggests that the history of the endemic thrasher and trembler lineage in the West Indies extends back about 4 Ma, and the three distinct clades of tremblers split about 2 Ma ago. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Missouri, Dept Biol, St Louis, MO 63121 USA. RP Hunt, JS (reprint author), Field Museum Nat Hist, Bird Div, Roosevelt Rd & Lake Shore Dr, Chicago, IL 60605 USA. NR 53 TC 57 Z9 58 U1 1 U2 7 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD JAN PY 2001 VL 118 IS 1 BP 35 EP 55 DI 10.1642/0004-8038(2001)118[0035:MSABOA]2.0.CO;2 PG 21 WC Ornithology SC Zoology GA 409TU UT WOS:000167402400005 ER PT J AU Marra, PP Holmes, RT AF Marra, PP Holmes, RT TI Consequences of dominance-mediated habitat segregation in American Redstarts during the nonbreeding season SO AUK LA English DT Article ID RADIO-TAGGED ANIMALS; MIGRATORY BIRD; POPULATION LIMITATION; SETOPHAGA-RUTICILLA; SEXUAL SELECTION; MIGRANT WARBLER; DYNAMICS; QUALITY; SURVIVAL; WINTER AB Several species of migratory songbirds exhibit a distinct form of habitat segregation while on their Neotropical wintering grounds in which males and females occupy different habitat types. In the American Redstart (Setophaga ruticilla), that sexual habitat segregation is a result of behavioral dominance of older males. In that study, we examined whether such dominance behavior and the resulting differential habitat segregation has consequences for the condition or survival of excluded individuals. We quantified the physical condition and survival of redstarts (both males and females) occupying two habitat types that differed in the proportion of males and females present in Jamaica. Both sexes of redstarts occupying female-biased habitat lost significantly more mass over-winter and had lower annual survival and longevity compared to individuals in male-biased habitat. These results suggest that nonbreeding habitats differed in suitability, with the least suitable habitat being occupied predominately by females. Because most female redstarts are forced to over-winter in these kinds of habitats, they may often be in poor physiological condition prior to departing on spring migration for the breeding grounds. This in turn may influence dynamics of the breeding period by determining their condition and perhaps reproductive success. Furthermore, because winter habitat segregation appears to lower female survivorship, it may also limit the number and availability of breeding females. These results implicate events that occur during the nonbreeding period as playing a critical role in the annual dynamics of this migratory species. C1 Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. RP Marra, PP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. NR 69 TC 153 Z9 157 U1 4 U2 32 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD JAN PY 2001 VL 118 IS 1 BP 92 EP 104 DI 10.1642/0004-8038(2001)118[0092:CODMHS]2.0.CO;2 PG 13 WC Ornithology SC Zoology GA 409TU UT WOS:000167402400008 ER PT J AU Lovette, IJ Bermingham, E AF Lovette, IJ Bermingham, E TI Mitochondrial perspective on the phylogenetic relationships of the Parula wood-warblers SO AUK LA English DT Article ID GENETIC DIFFERENTIATION; DENDROICA WARBLERS; TREE TOPOLOGIES; BIOGEOGRAPHY; TANAGERS; AVES C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. RP Lovette, IJ (reprint author), San Francisco State Univ, Dept Biol, Ctr Trop Res, 1600 Holloway Ave, San Francisco, CA 94132 USA. RI Lovette, Irby/P-3477-2014 NR 30 TC 19 Z9 23 U1 0 U2 0 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD JAN PY 2001 VL 118 IS 1 BP 211 EP 215 DI 10.1642/0004-8038(2001)118[0211:MPOTPR]2.0.CO;2 PG 5 WC Ornithology SC Zoology GA 409TU UT WOS:000167402400017 ER PT J AU Haggerty, TM Morton, ES Fleischer, RC AF Haggerty, TM Morton, ES Fleischer, RC TI Genetic monogamy in Carolina wrens (Thryothorus ludovicianus) SO AUK LA English DT Article ID EXTRA-PAIR PATERNITY; MIXED REPRODUCTIVE STRATEGIES; BREEDING SYNCHRONY; FERTILIZATIONS; BIRDS; CARE; DNA; POPULATIONS; BEHAVIOR C1 Univ N Alabama, Dept Biol, Florence, AL 35632 USA. Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Haggerty, TM (reprint author), Univ N Alabama, Dept Biol, Florence, AL 35632 USA. NR 29 TC 19 Z9 19 U1 2 U2 11 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD JAN PY 2001 VL 118 IS 1 BP 215 EP 219 DI 10.1642/0004-8038(2001)118[0215:GMICWT]2.0.CO;2 PG 5 WC Ornithology SC Zoology GA 409TU UT WOS:000167402400018 ER PT J AU Holtum, JAM Winter, K AF Holtum, JAM Winter, K TI Are plants growing close to the floors of tropical forests exposed to markedly elevated concentrations of carbon dioxide? SO AUSTRALIAN JOURNAL OF BOTANY LA English DT Article ID MONTANE RAIN-FOREST; ISOTOPE DISCRIMINATION; CO2; PHOTOSYNTHESIS; LEAVES; DELTA-C-13; PANAMA; GROWTH AB The study tested the frequently expressed perception that the concentration of CO2 in the vicinity of establishing seedlings growing close to tropical forest floors is generally high. CO2 concentration was monitored 10 cm from the forest floor over several days during wet and dry seasons at three Panamanian lowland and montane tropical forest sites. Air was sampled at a low flow rate with a peristaltic pump to minimise contamination by air from other strata. The average CO2 concentrations observed during the dry and wet seasons were 387 and 423 muL CO2 L-1 air, respectively, a relatively small enrichment compared with the above-canopy CO2 concentrations. The highest CO2 concentration recorded at 10 cm was 494 muL L-1. The generally modest levels of enrichment-far below concentrations required to saturate photosynthesis-were nonetheless sufficient to significantly increase the rates of CO2 uptake relative to above-canopy CO2 concentrations by shade-grown seedlings of Piper cordulatum C. DC., an understorey shrub and Virola surinamensis (Rol.) Warb., a late successional tree species. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. James Cook Univ N Queensland, Dept Trop Plant Sci, Townsville, Qld 4811, Australia. RP Holtum, JAM (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Ancon, Panama. RI Holtum, Joseph/B-3063-2012 OI Holtum, Joseph/0000-0001-6568-8019 NR 26 TC 11 Z9 11 U1 0 U2 5 PU C S I R O PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 0067-1924 J9 AUST J BOT JI Aust. J. Bot. PY 2001 VL 49 IS 5 BP 629 EP 636 DI 10.1071/BT00054 PG 8 WC Plant Sciences SC Plant Sciences GA 473VW UT WOS:000171070300011 ER PT J AU Jennions, MD Polakow, DA AF Jennions, MD Polakow, DA TI The effect of partial brood loss on male desertion in a cichlid fish: an experimental test SO BEHAVIORAL ECOLOGY LA English DT Article DE brood reduction; brood size; cichlids; mate desertion; parental care; life-history trade-off; mating opportunities ID ST PETERS FISH; WARBLERS ACROCEPHALUS-ARUNDINACEUS; MATE DESERTION; PARENTAL CARE; CICHLASOMA-NIGROFASCIATUM; PATERNAL CARE; FILIAL CANNIBALISM; CONVICT CICHLIDS; SNAIL KITE; SEX-RATIO AB There is little experimental evidence testing whether current brood size and past brood mortality influence mate desertion. In the cichlid Aequidens coeruleopunctatus both parents initially defend offspring. In a field study, all experimental broods, irrespective of initial brood size (222.9 +/- 60.4, mean +/- SD), were manipulated to a size of 100 fry. Neither the duration nor investment of females in parental care differed between control and brood reduced pairs, even though care seemed costly. On average, females lost 5.1 +/- 4.8% of initial weight while guarding a brood until independence. In contrast, males with experimentally reduced broods guarded fry for significantly fewer days before deserting their mate than did males from control pairs,vith natural-sized broods (20.5 +/- 7.5 vs. 14.2 +/- 6.2 days). In at least 20% of cases (n = 9/45), the deserting male immediately mated with another female. Males with experimentally reduced broods also spent less rime guarding fry before deserting and attacked fewer brood predators than did males with control broods. For broods manipulated to have 100 fry, there was a significant negative relationship between the days until male desertion and the proportion of the initial brood removed. This indicates that male assessment of the future success of the current brood (hence its reproductive value) is based on past mortality and/or that there is variation among males in the expected size of future broods. Both current brood size and brood size relative to initial brood size are therefore predictors of male, but not female, parental behavior and mate desertion. Female care may be unaffected by brood reduction due to limited breeding opportunities and partial compensation for reduced male care. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. Univ Cape Town, Dept Stat Sci, ZA-7701 Cape Town, South Africa. RP Jennions, MD (reprint author), Australian Natl Univ, Div Bot & Zool, Canberra, ACT 0200, Australia. RI Jennions, Michael/C-7560-2009 OI Jennions, Michael/0000-0001-9221-2788 NR 84 TC 29 Z9 29 U1 0 U2 11 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 J9 BEHAV ECOL JI Behav. Ecol. PD JAN-FEB PY 2001 VL 12 IS 1 BP 84 EP 92 PG 9 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 387ZB UT WOS:000166152000012 ER PT S AU Faden, RB AF Faden, RB BE Friis, I Ryding, O TI The Commelinaceae of Northeast Tropical Africa (Eritrea, Ethiopia, Djibouti, Somalia and Kenya): Diversity and phytogeography SO BIODIVERSITY RESEARCH IN THE HORN OF AFRICA REGION SE BIOLOGISKE SKRIFTER LA English DT Proceedings Paper CT 3rd International Symposium on the Flora of Ethiopia and Eritrea CY AUG 25-27, 1999 CL CARLBERG ACAD, COPENHAGEN, DENMARK SP Danish Nat Sci Res Council, Danish Council Dev Res, Carlsberg Fdn HO CARLBERG ACAD AB Northeast Tropical Africa (NETA, comprising Eritrea, Ethiopia, Djibouti, Somalia and Kenya) is rich in Commelinaceae, with 95 species in 10 genera. Twenty-four species, all belonging to Aneilema, Commelina or Cyanotis, are endemic to the region, with country rates of endemism ranging from zero to 35%. Three of the six sections of Aneilema a present in NETA have endemic species there, including section Somaliensia, which is wholly endemic to NETA. The forest genera of Commelinaccae in NETA comprise only 4% of the total species. NETA is richer in Commelinaceae than West Tropical Africa or Southern Africa. The most strongly represented flora element is the Somali-Masai flora element. NETA shares 12-13 species with the Arabian Peninsula and 14 species with India. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Systemat Biol, Washington, DC 20560 USA. RP Faden, RB (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Systemat Biol, Washington, DC 20560 USA. EM faden.robert@nmnh.si.edu NR 37 TC 2 Z9 2 U1 0 U2 1 PU ROYAL DANISH ACADEMY SCIENCES & LETTERS PI COPENHAGEN V PA H C ANDERSENS BLVD 35, DK-1553 COPENHAGEN V, DENMARK SN 0366-3612 BN 87-7876-246-4 J9 BIOL SKRIF PY 2001 VL 54 BP 213 EP 231 PG 19 WC Agronomy; Plant Sciences SC Agriculture; Plant Sciences GA BV38A UT WOS:000178753600015 ER PT J AU Spindler, RE Howard, J Huang, Y Li, DS Zhang, HM Wild, DE AF Spindler, RE Howard, J Huang, Y Li, DS Zhang, HM Wild, DE TI Cryopreservation has no impact on subsequent sperm capacitation in vitro in the giant panda. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA USA. China Res & Conservat Ctr Giant Panda, Wolong Nat Reserve, Peoples R China. NR 0 TC 1 Z9 1 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2001 VL 64 SU 1 BP 311 EP 312 PG 2 WC Reproductive Biology SC Reproductive Biology GA 447KR UT WOS:000169570900574 ER PT B AU Peitz, J AF Peitz, J BE Kaper, L VandenHeuvel, EPJ Woudt, PA TI Causal model for relativistic accretion flow SO BLACK HOLES IN BINARIES AND GALACTIC NUCLEI: DIAGNOSTICS, DEMOGRAPHY AND FORMATION SE ESO ASTROPHYSICS SYMPOSIA LA English DT Proceedings Paper CT ESO International Workshop on Black Holes in Binaries and Galactic Nuclei - Diagnostics, Demography and Formation CY SEP 06-08, 1999 CL GARCHING, GERMANY SP ESO AB Accretion onto compact objects is a prominent astrophysical problem involving dissipative fluid flow in strong gravitational fields. The generic approach for modeling is by the relativistic Navier-Stokes-Fourier equations, which are of nonhyperbolic type. Consequently, fluctuations in the dissipative variables (shear stress and heat flux) propagate at causality violating infinite speeds, and thermodynamic equilibrium states are unstable. This description is problematic in particular for systems that undergo variability on timescales shorter than or comparable to the dissipative relaxation times. To overcome these difficulties we proposed (Peitz & Appl [3]) to model relativistic accretion flows using extended causal fluid theories. Here we review such a theory and the corresponding 3+1 representation appropriate for numerical implementation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Peitz, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-41581-5 J9 ESO ASTROPHY SYMP PY 2001 BP 228 EP 229 DI 10.1007/10720995_49 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS56M UT WOS:000170337400049 ER PT B AU Kalogera, V AF Kalogera, V BE Kaper, L VandenHeuvel, EPJ Woudt, PA TI Formation of black-hole X-ray binaries with low-mass donors SO BLACK HOLES IN BINARIES AND GALACTIC NUCLEI: DIAGNOSTICS, DEMOGRAPHY AND FORMATION SE ESO ASTROPHYSICS SYMPOSIA LA English DT Proceedings Paper CT ESO International Workshop on Black Holes in Binaries and Galactic Nuclei - Diagnostics, Demography and Formation CY SEP 06-08, 1999 CL GARCHING, GERMANY SP ESO ID STARS AB The characteristics of black-hole X-ray binaries can be used to obtain information about their evolutionary history and the process of black-hole formation. In this paper I focus on systems with donor masses lower than the inferred black-hole masses. Current models for the evolution of hydrogen-rich, massive stars and of helium stars losing mass in a wind cannot explain the current sample of black-hole mass measurements. Assuming that the radial evolution of mass-losing massive stars is at least qualitatively accurate, I show that the properties of the BH companions lead to constraints on the masses of black-hole progenitors (at most twice the black-hole mass) and on the strength of winds in helium stars (fractional amount of mass lost smaller than about 50%). Constraints on common-envelope evolution are also derived. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vkalogera@cfa.harvard.edu NR 11 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-41581-5 J9 ESO ASTROPHY SYMP PY 2001 BP 299 EP 304 DI 10.1007/10720995_65 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS56M UT WOS:000170337400065 ER PT J AU Wilczynski, W Rand, AS Ryan, MJ AF Wilczynski, W Rand, AS Ryan, MJ TI Evolution of calls and auditory tuning in the Physalaemus pustulosus species group SO BRAIN BEHAVIOR AND EVOLUTION LA English DT Article DE Amphibian; Tungara frog; auditory; amphibian papilla; basilar papilla; acoustic communication; sensory exploitation ID SEXUAL SELECTION; CRICKET FROGS; ACOUSTIC COMMUNICATION; ANIMAL COMMUNICATION; SENSORY EXPLOITATION; AMPHIBIAN PAPILLA; RANA-CATESBEIANA; NEOTROPICAL FROG; RECEIVER BIASES; ACRIS-CREPITANS AB In species within the Physalaemus pustulosus species group, male frogs produce a whine-like advertisement call consisting of a frequency sweep typically descending from 1,000 to 400 Hz (depending on the species). One species, Physalaemus pustulosus, the tungara frog, has evolved a second call syllable, the chuck, which males place after their whine. Most energy in the chuck is above 1,500 Hz and peaks at 2,400 Hz. We investigated whether the evolution of this new call component in P. pustulosus coincided with evolution of auditory tuning. We used multiunit electrophysiological recordings of auditory-evoked activity in the midbrain to characterize auditory tuning in Physalaemus pustulosus, four other Physalaemus species within the P. pustulosus clade, and three additional, closely related Physalaemus species as outgroups. All eight species had similar sensitivity profiles, with a broad area of enhanced sensitivity from 100 to 1,100 Hz, which we presume represents amphibian papilla (AP) tuning, and a second, narrower area of enhanced sensitivity centered above 2,100 Hz, which we presume represents basilar papilla (BP) tuning. For all species, the whine stimulates the AP. The P. pustulosus chuck stimulates the BP. The frequency with greatest AP sensitivity differed significantly among species. Although in all cases the AP peak lay within the frequency sweep of the whine, phylogenetically corrected correlations revealed no significant relationships between AP tuning and any spectral feature of the whine. BP tuning was similar among all species, with mean BP best excitatory frequencies (BEFs) around 2,1002,200 Hz, with the exception of P. pustulatus, with a mean BP BEF of 2,549 Hz. Physalaemus pustulosus, the only investigated species that produces a call component stimulating the BP, had a BP BEF that was not significantly different from any of the species within its clade except P. pustulatus, or from any of the outgroup species. A phylogenetic reconstruction of ancestral BP tuning confirms that the only point of evolutionary change in BP tuning is in the line of descent leading to P. pustulatus, not in the line leading to P. pustulosus despite this being the species using the BP for communication. The results indicate that BP tuning around 2,200 Hz is a conserved trait in the Physalaemus pustulosus species group and that no evolution of BP tuning accompanied the subsequent evolution of the call component (the chuck) that stimulates it. This supports the sensory exploitation idea, which posits that signals evolve to match preexisting features of receiver systems. C1 Univ Texas, Dept Psychol, Austin, TX 78712 USA. Univ Texas, Inst Neurosci, Austin, TX 78712 USA. Smithsonian Trop Res Inst, Balboa, Panama. Univ Texas, Sect Integrat Biol, Austin, TX 78712 USA. RP Wilczynski, W (reprint author), Univ Texas, Dept Psychol, 330 Mezes Hall, Austin, TX 78712 USA. NR 70 TC 55 Z9 58 U1 1 U2 9 PU KARGER PI BASEL PA ALLSCHWILERSTRASSE 10, CH-4009 BASEL, SWITZERLAND SN 0006-8977 J9 BRAIN BEHAV EVOLUT JI Brain Behav. Evol. PY 2001 VL 58 IS 3 BP 137 EP 151 DI 10.1159/000047268 PG 15 WC Behavioral Sciences; Neurosciences; Zoology SC Behavioral Sciences; Neurosciences & Neurology; Zoology GA 531ND UT WOS:000174420700002 PM 11910171 ER PT J AU Blanco, JG Duckett, CN AF Blanco, JG Duckett, CN TI Taxonomic revision and cladistic analysis of Homoschema Blake (Coleoptera : Chrysomelidae : Alticinae) SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article ID BEETLES AB The West Indian genus Homoschema Blake is revised and redescribed. Seven new species are described: H, biscutatum (Hispaniola), H. blakeae (Jamaica), a furthi (Dominican Republic), H, lineatum (Dominica), H. lingulatum (Dominican Republic), H. pseudobuscki (Jamaica), and H. sasha (Cuba). Twenty species are redescribed: H. androsense Blake (Bahama Islands), H. azureipenne Bechyne (Guadeloupe), H. buscki Blake (Hispaniola), H. dominicae Blake (Dominica), H, felis Blake (Bahama Islands), H. fraternum Blake (Puerto Rico), H, hoffmani Blake (Hispaniola), H, jamaicense Blake (Jamaica), H. latitarsum Blake (Puerto Rico), H. latum Blake (Cuba), H. leucurum Blake (Hispaniola), H. longense Blake (Bahama Islands), H. manni Blake (Cuba), H. nigriventre Blake (Puerto Rico), H. obesum Blake (Puerto Rico), H. opimum Blake (Hispaniola), a orientense Blake (Cuba), H, ornatum Blake (Cuba), H. pingue Blake (St. Croix, V.I.), and H. xanthocyaneum Blake (Jamaica). A key to the species is provided. A cladistic analysis based on 16 morphological characters of adults from 29 taxa supports the monophyly of Homoschema. Cladograms indicate several evolutionary patterns involving the head capsule, pronotum, and the genitalia of both sexes. Phylogenetic relationships among some Homoschema species are unresolved in all equally parsimonious trees. C1 Univ Puerto Rico, Dept Biol, Mayaguez, PR 00681 USA. Univ Puerto Rico, Dept Biol, San Juan, PR 00931 USA. RP Blanco, JG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. EM blanco.javier@nmnh.si.edu; catherineduckett@hotmail.com NR 28 TC 2 Z9 4 U1 1 U2 1 PU UNIV PUERTO RICO, PI MAYAGUEZ PA COLLEGE ARTS SCIENCES, MAYAGUEZ, PR 00680 USA SN 0008-6452 J9 CARIBB J SCI JI Caribb. J. Sci. PY 2001 VL 37 IS 1-2 BP 1 EP 29 PG 29 WC Biodiversity Conservation SC Biodiversity & Conservation GA 439XM UT WOS:000169142900001 ER PT J AU Zusi, RL Hamas, MJ AF Zusi, RL Hamas, MJ TI Bats and birds as potential pollinators of three species of Marcgravia lianas on Dominica SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article ID FOREST C1 Natl Museum Nat Hist, Dept Systemat Biol, Smithsonian Inst, Washington, DC 20560 USA. Cent Michigan Univ, Dept Biol, Mt Pleasant, MI 48858 USA. RP Zusi, RL (reprint author), Natl Museum Nat Hist, Dept Systemat Biol, Smithsonian Inst, Washington, DC 20560 USA. EM zusir@nmnh.si.edu NR 19 TC 8 Z9 8 U1 1 U2 2 PU UNIV PUERTO RICO, PI MAYAGUEZ PA COLLEGE ARTS SCIENCES, MAYAGUEZ, PR 00680 USA SN 0008-6452 J9 CARIBB J SCI JI Caribb. J. Sci. PY 2001 VL 37 IS 3-4 BP 274 EP 278 PG 5 WC Biodiversity Conservation SC Biodiversity & Conservation GA 498GQ UT WOS:000172501800016 ER PT S AU Wildt, DE Howard, J Brown, J AF Wildt, DE Howard, J Brown, J BE Gittleman, JL Funk, SM Macdonald, DW Wayne, RK TI Role of reproductive sciences in carnivore conservation SO CARNIVORE CONSERVATION SE CONSERVATION BIOLOGY SERIES LA English DT Proceedings Paper CT Meeting on Carnivore Conservation CY NOV 20-21, 1998 CL ZOOL SOC LONDON, LONDON, ENGLAND HO ZOOL SOC LONDON C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Wildt, DE (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. NR 0 TC 10 Z9 10 U1 1 U2 2 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1363-3090 BN 0-521-66232-X J9 CONSERV BIOL SER PY 2001 VL 5 BP 359 EP 371 PG 13 WC Biodiversity Conservation; Zoology SC Biodiversity & Conservation; Zoology GA BS76S UT WOS:000171058900016 ER PT B AU Barth, AJ Sarzi, M Ho, LC Rix, HW Shields, JC Filippenko, AV Rudnick, G Sargent, WLW AF Barth, AJ Sarzi, M Ho, LC Rix, HW Shields, JC Filippenko, AV Rudnick, G Sargent, WLW BE Knapen, JH Beckman, JE Shlosman, I Mahoney, TJ TI Measuring black-hole masses using ionized-gas kinematics SO CENTRAL KILOPARSEC OF STARBURSTS AND AGN: THE LA PALMA CONNECTION SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on the Central Kiloparsec of Starbursts and AGN CY MAY 07-11, 2001 CL LOS CANCAJOS, SPAIN SP Isaac Newton Grp Telescopes AB We describe techniques for measuring the central masses of galaxies using emission-line kinematics observed with the Hubble Space Telescope. For accurate results, it is necessary to model various instrumental effects, particularly the blurring due to the telescope PSF and the width of the spectroscopic aperture. Observations of nuclear gas disks often reveal substantial internal velocity dispersions in the gas, suggesting that the disks may be partially pressure-supported. We also describe a technique for fitting two-dimensional spectroscopic data directly in pixel space. This method may be useful for objects such as M84 that show highly complex and asymmetric line profiles. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. RP Barth, AJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 01238 USA. NR 8 TC 6 Z9 6 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-089-7 J9 ASTR SOC P PY 2001 VL 249 BP 370 EP 374 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU54V UT WOS:000176290900048 ER PT B AU Zezas, A Fabbiano, G Prestwich, A Murray, S Ward, M AF Zezas, A Fabbiano, G Prestwich, A Murray, S Ward, M BE Knapen, JH Beckman, JE Shlosman, I Mahoney, TJ TI Chandra observations of the stellar populations and diffuse gas in nearby galaxies SO CENTRAL KILOPARSEC OF STARBURSTS AND AGN: THE LA PALMA CONNECTION SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on the Central Kiloparsec of Starbursts and AGN CY MAY 07-11, 2001 CL LOS CANCAJOS, SPAIN SP Isaac Newton Grp Telescopes ID X-RAY SOURCES; BLACK-HOLES; STARBURST AB We present Chandra observations of two star-forming galaxies (M82 and The Antennae) and three starburst/AGN composite galaxies (NGC 1808, NGC 6240, and NGC 7331). In both star-forming galaxies we detect a large number of sources with diverse properties. Some of them can be identified as X-ray binaries, based on their variability and spectra. However, there is a significant number of very soft and/or extended sources which could be supernova remnants. These observations confirm previous indications that there is a population of sources with X-ray luminosities much higher than the Eddington limit for a neutron star, suggesting that these objects are abundant in star-forming galaxies. We find that the X-ray luminosity functions of the discrete sources in these two galaxies are very similar. In the case of the composite galaxies we find that the AGN do not dominate their X-ray emission. A significant fraction of the emission from these objects is extended but there are also X-ray sources associated with circumnuclear star-formation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zezas, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 17 TC 14 Z9 14 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-089-7 J9 ASTR SOC P PY 2001 VL 249 BP 425 EP 431 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU54V UT WOS:000176290900055 ER PT B AU Sakamoto, K Fukuda, H Wada, K Habe, A AF Sakamoto, K Fukuda, H Wada, K Habe, A BE Knapen, JH Beckman, JE Shlosman, I Mahoney, TJ TI Molecular gas in the central kpc of m81 SO CENTRAL KILOPARSEC OF STARBURSTS AND AGN: THE LA PALMA CONNECTION SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on the Central Kiloparsec of Starbursts and AGN CY MAY 07-11, 2001 CL LOS CANCAJOS, SPAIN SP Isaac Newton Grp Telescopes ID SUPERMASSIVE BLACK-HOLE; NUCLEUS AB We observed the central kpc of M81 in CO (1-->0) and 3 mm continuum at 100 pc resolution in order to probe molecular gas and to search for the nuclear inner Lindblad resonance around the low-luminosity AGN M81*. Most molecular gas in the region is in the "pseudo-ring" at a radius of similar to 500 pc. The region within 300 pc from the nucleus, where the resonance is expected, has no CO emission. The resonance was thus not found. The 3 mm continuum from the nucleus showed intraday variation, and no CO absorption against the continuum was detected. C1 Harvard Smithsonian Ctr Astrophys, Hilo, HI 96721 USA. RP Sakamoto, K (reprint author), Harvard Smithsonian Ctr Astrophys, POB 824, Hilo, HI 96721 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-089-7 J9 ASTR SOC P PY 2001 VL 249 BP 707 EP 710 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU54V UT WOS:000176290900098 ER PT B AU Matsushita, S Kawabe, R Matsumoto, H Tsuru, TG Kohno, K Vila-Vilaro, B AF Matsushita, S Kawabe, R Matsumoto, H Tsuru, TG Kohno, K Vila-Vilaro, B BE Knapen, JH Beckman, JE Shlosman, I Mahoney, TJ TI Molecular gas in M82: Superbubble, starburst, and massive black hole SO CENTRAL KILOPARSEC OF STARBURSTS AND AGN: THE LA PALMA CONNECTION SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on the Central Kiloparsec of Starbursts and AGN CY MAY 07-11, 2001 CL LOS CANCAJOS, SPAIN SP Isaac Newton Grp Telescopes ID SCALE AB We performed deep (CO)-C-12 (1-->0) interferometric observations of the starburst galaxy M82 with the Nobeyama Millimeter Array. We have successfully imaged an expanding molecular superbubble with a diameter of about 200 pc (about 14") and a kinetic energy of about 10(55) erg. The center of the superbubble is clearly shifted from the nucleus by 140 pc. This position is close to those of the intermediate-mass black hole (BH) and the 2.2 mum secondary peak. Calculations of the stellar population in the 2.2 mum secondary peak cluster based on a usual initial mass function for starburst galaxies suggest that it may be possible to form an intermediate-mass BH with stellar-stellar or BH-BH mergers. Our results may give a new explanation to the starburst-AGN connection. C1 Harvard Smithsonian Ctr Astrophys, Hilo, HI 96721 USA. RP Matsushita, S (reprint author), Harvard Smithsonian Ctr Astrophys, POB 824, Hilo, HI 96721 USA. NR 14 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-089-7 J9 ASTR SOC P PY 2001 VL 249 BP 711 EP 714 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU54V UT WOS:000176290900099 ER PT J AU Pasteels, JM Termonia, A Windsor, DM Witte, L Theuring, C Hartmann, T AF Pasteels, JM Termonia, A Windsor, DM Witte, L Theuring, C Hartmann, T TI Pyrrolizidine alkaloids and pentacyclic triterpene saponins in the defensive secretions of Platyphora leaf beetles SO CHEMOECOLOGY LA English DT Article DE alkaloid sequestration; chemical defense; Platyphora leaf beetles; pyrrolizidine alkaloids; triterpene saponins ID MECHANITIS-POLYMNIA LEPIDOPTERA; CHEMICAL DEFENSE; SEQUESTRATION; BIOSYNTHESIS; METABOLISM; ITHOMIINAE; TRANSFORMATION; BUTTERFLIES; NYMPHALIDAE; STORAGE AB Field collected exocrine defensive secretions of nine neotropical Platyphora species were analyzed for the presence of plant acquired pyrrolizidine alkaloids (PAs) and pentacyclic triterpene saponins. All species secrete saponins. In addition, five species feeding on Tournefortia (Boraginaceae), Koanophyllon (Asteraceae, tribe Eupatorieae) and Prestonia (Apocynaceae) were shown to sequester PAs of the lycopsamine type, which are characteristic for species of the three plant families. The PA sequestering species commonly store intermedine, lycopsamine and their O-3'-acetyl or propionyl esters as well as O-7- and O-9-hydroxyisovaleryl esters of retronecine. The latter as well as the O-3-acyl esters were not found in the beetles' host plants, suggesting the ability of the beetles to esterify plant derived retronecine and intermedine or its stereoisomers. Despite the conformity of the beetles' PA patterns, considerable inconsistencies exist regarding the PA patterns of the respective host plants. One host plant was devoid of PAs, while another contained only simple necines. Since the previous history of the field collected beetles was unknown this discrepancy remains obscure. In contrast to the Palearctic chrysomeline leaf beetles, e.g. some Oreina species which ingest and store PAs as their non-toxic N-oxides, Platyphora leaf beetles absorb and store PAs as the toxic free base (tertiary PA), but apparently avoid to accumulate PAs in the haemolymph. This suggests that Chrysolina and Platyphora leaf beetles developed different lines of adaptations in their parallel evolution of PA mediated chemical defense. C1 Free Univ Brussels, Lab Anim & Cellular Biol, B-1050 Brussels, Belgium. Univ Brussels, Inst Mol Biol & Med, Unit Evolutionary Genet, B-6041 Gosselies, Belgium. Smithsonian Trop Res Inst, Balboa, Panama. Tech Univ Carolo Wilhelmina Braunschweig, Inst Pharmazeut Biol, D-38106 Braunschweig, Germany. RP Pasteels, JM (reprint author), Free Univ Brussels, Lab Anim & Cellular Biol, POB 160-12,50 Av FD Roosevelt, B-1050 Brussels, Belgium. NR 29 TC 33 Z9 34 U1 1 U2 6 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0937-7409 J9 CHEMOECOLOGY JI Chemoecology PY 2001 VL 11 IS 3 BP 113 EP 120 DI 10.1007/PL00001840 PG 8 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 482GF UT WOS:000171567700002 ER PT J AU Vardi, A Shapiro, M AF Vardi, A Shapiro, M TI Theory of laser catalysis with pulses SO COMMENTS ON MODERN PHYSICS LA English DT Article DE laser catalysis; laser modified tunneling; light induced potentials; reactive scattering; exchange reactions; resonant tunneling ID POTENTIAL-ENERGY SURFACE; SCANNING TUNNELING MICROSCOPE; 3-DIMENSIONAL QUANTUM-THEORY; FABRY-PEROT-INTERFEROMETER; INDUCED CHEMICAL-REACTIONS; LI+HCL REACTION; DOUBLE-BARRIER; MOLECULAR-COLLISIONS; EXCHANGE-REACTION; COHERENT CONTROL AB The possibility of accelerating molecular reactions by lasers has attracted considerable theoretical and experimental interest. A particular example of laser-modified reaction dynamics is laser catalysis, a process in which the tunneling through a potential barrier is enhanced by transient excitation to a bound electronic state. We have performed detailed calculations of pulsed laser catalysis on one- and two-dimensional potentials, as a function of the reactants' collision energy and the laser's central frequency. In agreement with previous CW results, the reactive lineshapes are Fano-type curves, resulting from interference between nonradiative tunneling and the optically assisted pathway. In contrast to the CW process, the power requirements of pulsed laser catalysis are well within the reach of commonly used pulsed laser sources, making an experimental realization possible. The laser catalysis scenario is shown to be equivalent in the "dressed" state picture, to resonant tunneling through a double-barrier potential, admitting perfect transmission when the incident energy matches a quasibound state of the well within the barriers. Possible applications for atom optics, solid-state devices, and scanning tunneling microscopy, are discussed. C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Weizmann Inst Sci, Dept Chem Phys, IL-76100 Rehovot, Israel. RP Vardi, A (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St,MS14, Cambridge, MA 02138 USA. RI Vardi, Amichay/D-8189-2011 OI Vardi, Amichay/0000-0002-8992-2129 NR 79 TC 6 Z9 6 U1 1 U2 2 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK,, ABINGDON OX14 4RN, OXON, ENGLAND SN 1560-5892 J9 COMMENT MOD PHYS JI Comment Mod. Phys. PY 2001 VL 2 IS 5 BP D233 EP D244 PG 12 WC Physics, Multidisciplinary SC Physics GA 506QF UT WOS:000172982700007 ER PT B AU Shurgalin, M Murray, AJ MacGillivray, WR Standage, MC AF Shurgalin, M Murray, AJ MacGillivray, WR Standage, MC BE Becker, U Crowe, A TI The transfer of angular momentum for electron-atom collision processes involving inelastically excited S -> P and P -> S transitions SO COMPLETE SCATTERING EXPERIMENTS SE PHYSICS OF ATOMS AND MOLECULES LA English DT Proceedings Paper CT Han Kleinpoppen Symposium on Complete Scattering Experiments CY 1998 CL CIOCCO, ITALY SP Royal Soc London, Max Planck Gesell ID ORIENTATION; ALIGNMENT; IMPACT; EXCITATION AB Since the initial electron-photon coincidence and superelastic scattering experiments showed that substantial transfers of angular momentum between incident electrons and target atoms could occur, apart from stimulating much theoretical activity to develop better quantum mechanical scattering calculations, several classical/semi-classical models have also been developed. In this paper, new experimental results from electron inelastic scattering from the laser excited 3(2)P(3/2) state of sodium has provided a further test of scattering theories, including a very recent convergent close coupling calculation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Shurgalin, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU KLUWER ACADEMIC/PLENUM PUBL PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA BN 0-306-46503-5 J9 PHYS ATOMS PY 2001 BP 129 EP 137 PG 9 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA BS20J UT WOS:000169067300005 ER PT J AU Du Foresto, VC Chagnon, G Lacasse, M Mennesson, B Morel, S Perrin, G Ridgway, S Traub, W AF Du Foresto, VC Chagnon, G Lacasse, M Mennesson, B Morel, S Perrin, G Ridgway, S Traub, W TI The FLUOR interferometric beam combiner SO COMPTES RENDUS DE L ACADEMIE DES SCIENCES SERIE IV PHYSIQUE ASTROPHYSIQUE LA English DT Article DE interferometry; aperture synthesis; high angular resolution; guided optics; stellar astrophysics ID IOTA INTERFEROMETER; STELLAR; INSTRUMENT; OPTICS AB FLUOR stands for Fibered Linked Unit for Optical Recombination and is an interferometric instrument which started out as a technology demonstrator, demonstrated the potential of single-mode fiber optics fur high precision visibility measurements, and has been operated as a focal instrument of the IOTA interferometer since 1995. After a presentation of the instrument, the programs carried out with FLUOR are reviewed, as well as the perspectives introduced by interferometric observations with a high dynamic range. (C) 2001 Academie des sciences/Editions scientifiques et medicales Elsevier SAS. C1 Observ Paris, DESPA, F-92195 Meudon, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Du Foresto, VC (reprint author), Observ Paris, DESPA, F-92195 Meudon, France. NR 30 TC 4 Z9 4 U1 0 U2 0 PU EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS CEDEX 15 PA 23 RUE LINOIS, 75724 PARIS CEDEX 15, FRANCE SN 1296-2147 J9 CR ACAD SCI IV-PHYS JI C. R. Acad. Sci. Ser. IV-Phys. Astrophys. PD JAN-FEB PY 2001 VL 2 IS 1 BP 45 EP 55 PG 11 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA 416FH UT WOS:000167769300006 ER PT B AU Hartmann, L AF Hartmann, L BE Lopez, RJG Rebolo, R Osorio, MRZ TI Pre-main sequence evolution of low-mass stars SO COOL STARS, STELLAR SYSTEMS AND THE SUN, PROCEEDINGS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 11th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY OCT 04-08, 1999 CL PUERTO LA CRUZ, SPAIN SP Spains Minist Educ & Cultura, Univ La Laguna, Cabildo Tenerife, Canaries Local Govt ID T-TAURI STARS; YOUNG STELLAR OBJECTS; MAGNETOSPHERIC ACCRETION MODELS; AURIGA MOLECULAR CLOUD; BALMER LINE-PROFILES; DISK ACCRETION; CIRCUMSTELLAR DISKS; MAGNETIC-FIELD; HR 4796A; JETS AB I summarize progress, as well as outstanding problems, in three areas of pre-main sequence evolution: the time-variability of disk accretion, and the related possibility of forming binaries as well as planets in disks; the coupling between magnetic fields and disk material, which accounts for powerful jets and truncates the inner regions of T Tauri disks, and probably spins down the central star; and the ending of disk accretion at the epoch of planet formation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hartmann, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 71 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-056-0 J9 ASTR SOC P PY 2001 VL 223 BP 3 EP 18 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS48R UT WOS:000170040600001 ER PT B AU Saar, SH AF Saar, SH BE Lopez, RJG Rebolo, R Osorio, MRZ TI Recent measurements of (and inferences about) magnetic fields on K and M stars SO COOL STARS, STELLAR SYSTEMS AND THE SUN, PROCEEDINGS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 11th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY OCT 04-08, 1999 CL PUERTO LA CRUZ, SPAIN SP Spains Minist Educ & Cultura, Univ La Laguna, Cabildo Tenerife, Canaries Local Govt ID ORBITAL PERIOD MODULATION; ACTIVITY CYCLE PERIOD; MAIN-SEQUENCE STARS; T-TAURI STARS; CLOSE BINARIES; TIME EVOLUTION; FLUX; EMERGENCE; ROTATION; MODELS AB I review recent progress in measuring magnetic fields in K and M stars, including new detections (including T Tauri's), new observational and modeling methods, and new insight (from various sources) on the nature and evolution of magnetic regions on cool stars. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Saar, SH (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 49 TC 49 Z9 50 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-056-0 J9 ASTR SOC P PY 2001 VL 223 BP 292 EP 299 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS48R UT WOS:000170040600026 ER PT B AU Golub, L AF Golub, L BE Lopez, RJG Rebolo, R Osorio, MRZ TI Recent results from TRACE SO COOL STARS, STELLAR SYSTEMS AND THE SUN, PROCEEDINGS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 11th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY OCT 04-08, 1999 CL PUERTO LA CRUZ, SPAIN SP Spains Minist Educ & Cultura, Univ La Laguna, Cabildo Tenerife, Canaries Local Govt ID TRANSITION REGION; CORONAL EXPLORER; VIEW AB The TRACE Observatory is the first solar-observing satellite in the NASA Small Explorer series. Launched into a polar sun-synchronous orbit April 2, 1998, it is providing views of the solar transition region and low corona with unprecedented spatial and temporal resolution. The corona is now seen to be highly filamented, and filled with flows and other dynamic processes. Structure is seen down to the resolution limit of the instrument, while variability and motions are observed at all spatial locations in the solar atmosphere, and on very short timescales. Flares and shock waves are observed, and the spatial and temporal resolution are now adequate for a determination of how both the plasma and the magnetic fields evolve during a flare. The formation of long-lived coronal structures, with consequent implications for coronal heating models, has been seen. This overview describes the instrument and presents some results from the first 1-1/2 years of operation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Golub, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 13 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-056-0 J9 ASTR SOC P PY 2001 VL 223 BP 325 EP 332 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS48R UT WOS:000170040600029 ER PT B AU Dupree, AK AF Dupree, AK BE Lopez, RJG Rebolo, R Osorio, MRZ TI Coronal physics of cool stars SO COOL STARS, STELLAR SYSTEMS AND THE SUN, PROCEEDINGS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 11th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun CY OCT 04-08, 1999 CL PUERTO LA CRUZ, SPAIN SP Spains Minist Educ & Cultura, Univ La Laguna, Cabildo Tenerife, Canaries Local Govt ID RS-CANUM-VENATICORUM; EXTREME-ULTRAVIOLET-SPECTRUM; TRANSITION-REGION STRUCTURE; X-RAY SURVEY; AR-LACERTAE; STELLAR CORONAE; SYSTEM HR-1099; ENERGY-BALANCE; HYBRID STARS; V711 TAURI AB Spectroscopy from EUVE and ASCA has revealed the structure of stellar coronas in cool stars. These results demonstrate surprisingly different coronal structures from what is known on the Sun. Spectral diagnostics indicate small, hot, high density regions produced in rapidly rotating stellar atmospheres with some systems exhibiting phenomena that have no solar counterpart. Analysis suggests a continuous distribution of plasma temperature, a differential emission measure perhaps deviating from equilibrium assumptions, and high electron densities (10(12) - 10(13) cm(-3)). Unresolved aspects of the interpretations remain, among them metal abundances in stellar coronas, polar or high latitude structures in rapidly rotating stars, the presence or absence of extended coronal features, cool low-lying material, and demanding requirements for coronal heating. Recent observations of active systems from EUVE and ASCA illustrate these concepts; the Chandra spectra of Capella generally confirm these models and set the stage for spectroscopy of a larger coronal sample of cool stars with better resolution and increased effective area from Chandra, XMM, and ASTRO-E. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-15, Cambridge, MA 02138 USA. NR 53 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-056-0 J9 ASTR SOC P PY 2001 VL 223 BP 333 EP 350 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS48R UT WOS:000170040600030 ER PT J AU Littler, MM Littler, DS AF Littler, MM Littler, DS TI Living stromatolites, built by the cyanobacterium Schizothrix gebeleinii, form enduring modern reef structures SO CORAL REEFS LA English DT Article ID SUBTIDAL STROMATOLITES; BAHAMAS C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. Harbor Branch Oceanog Inst Inc, Div Marine Sci, Ft Pierce, FL 34946 USA. RP Littler, MM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. NR 4 TC 1 Z9 1 U1 0 U2 1 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD JAN PY 2001 VL 19 IS 3 BP 258 EP 258 DI 10.1007/PL00006960 PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 401EZ UT WOS:000166915500008 ER PT S AU Gingerich, O AF Gingerich, O BE Miller, JB TI Scientific cosmology meets western theology - A historical perspective SO COSMIC QUESTIONS SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Cosmic Questions CY APR, 1999 CL WASHINGTON, D.C. SP Dialogue Sci, Ethics & Relig, AAAS Program, John Templeton Fdn, Smithsonian Inst, Off Provost, Sci & Spirit Resources Inc, N Amer Montessori Teachers Assoc DE Copernican revolution; Johannes Kepler; Galileo; Edwin Hubble; Big Bang cosmology; Fred Hoyle; steady-state cosmology AB Traditional sacred geography of Christendom met a challenge not so much from Copernicus' heliocentrism per se as from the greatly explanded vision of the cosmos that it ushered in. The twentieth-century view of the vastness of both space and time has brought revolutionary conceptual changes to the sacred landscape. From a theistic perspective, God is not simply the source of the Big Bang, but the Creator in the larger sense of designer and intender of the universe. C1 Harvard Univ, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 17 TC 0 Z9 0 U1 1 U2 4 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-346-7 J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2001 VL 950 BP 28 EP 38 PG 11 WC Multidisciplinary Sciences; Philosophy SC Science & Technology - Other Topics; Philosophy GA BT92Q UT WOS:000174462800003 PM 11797757 ER PT S AU Latham, DW AF Latham, DW BE Miller, JB TI Homes for extraterrestrial life - Extrasolar planets SO COSMIC QUESTIONS SE ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article; Proceedings Paper CT Conference on Cosmic Questions CY APR, 1999 CL WASHINGTON, D.C. SP Dialogue Sci, Ethics & Relig, AAAS Program, John Templeton Fdn, Smithsonian Inst, Off Provost, Sci & Spirit Resources Inc, N Amer Montessori Teachers Assoc DE extrasolar planets; the solar system; Doppler spectroscopy; space astrometry ID COMPANION AB Astronomers are now discovering giant planets orbiting other stars like the sun by the dozens. But none of these appears to be a small rocky planet like the earth, and thus these planets are unlikely to be capable of supporting life as we know it. The recent discovery of a system of three planets is especially significant because it supports the speculation that planetary systems, as opposed to single orbiting planets, may be common. Our ability to detect extrasolar planets will continue to improve, and space missions now in development should be able to detect earth-like planets. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Latham, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 7 TC 0 Z9 0 U1 0 U2 3 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 EAST 63RD ST, NEW YORK, NY 10021 USA SN 0077-8923 BN 1-57331-346-7 J9 ANN NY ACAD SCI JI Ann.NY Acad.Sci. PY 2001 VL 950 BP 259 EP 268 PG 10 WC Multidisciplinary Sciences; Philosophy SC Science & Technology - Other Topics; Philosophy GA BT92Q UT WOS:000174462800021 PM 11797754 ER PT B AU Weldon, PJ Wheeler, JW AF Weldon, PJ Wheeler, JW BE Grigg, GC Seebacher, F Franklin, CE TI The chemistry of crocodilian skin glands SO CROCODILIAN BIOLOGY AND EVOLUTION LA English DT Proceedings Paper CT Conference on Crocodilian Biology and Evolution CY JUL, 1998 CL UNIV QUEENSLAND, ST LUCIA, AUSTRALIA SP Univ Queensland, Dept Zool HO UNIV QUEENSLAND ID ALLIGATOR ALLIGATOR-MISSISSIPPIENSIS; THIN-LAYER CHROMATOGRAPHY; PARACLOACAL GLANDS; REPTILIAN CHEMISTRY; CITRONELLYL ESTERS; SECRETIONS; LIPIDS; CAIMAN; DIANEACKERONE; TRIGONATUS AB All modern crocodillans possess two prominent pairs of skin glands, the gular glands, which are located on the ventral surface of the lower jaw, and the paracloacal glands, which are embedded in the walls of the cloaca. These organs are thought to secrete pheromones used in mating or nesting activities. Analyses by thin-layer chromatography (TLC) of the glandular secretions indicate inter-gland, sex, taxonomic, and possibly individual variation In lipid composition. Sterols, free fatty acids, steryl esters, and other compound classes are suggested by TLC. Analyses by gas chromatography/mass spectrometry and other methods elucidate the structures of glandular components and reveal sex and age-class variation in secretion composition. The gular glands of the American alligator Alligator mississippiensis secrete squalene, cholesterol, free fatty acids, and alpha-tocopherol (vitamin E). The paracloacal glands of various crocodillans secrete hydrocarbons, steroids, free fatty acids, alcohols, ketones, and an array of esters. Some paracloacal gland compounds, such as citronellol from caimans (Caiman spp. and Paleosuchus spp.), are not known from other vertebrates. Other compounds, such as the aromatic ketone dianeackerone and a family of related steryl esters from the African dwarf crocodile Osteolaemus tetraspis, are known from no other natural source. Both the gular and the paracloacal glands form secretions when parenchymal cells lyse and discharge their contents as they migrate toward the Centre of the glands. Circulatory and lymphatic elements extending Into the glands also may contribute compounds to the exudates. C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Weldon, PJ (reprint author), Smithsonian Inst, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. NR 33 TC 3 Z9 3 U1 2 U2 8 PU SURREY BEATTY & SONS PI CHIPPING NORTON NSW PA 32 RICKARD ROAD, CHIPPING NORTON NSW, 2170, AUSTRALIA BN 0-949324-89-2 PY 2001 BP 286 EP 296 PG 11 WC Ecology; Developmental Biology; Zoology SC Environmental Sciences & Ecology; Developmental Biology; Zoology GA BT71L UT WOS:000173832900023 ER PT S AU Lukin, M Fleischhauer, M Imamoglu, A AF Lukin, M Fleischhauer, M Imamoglu, A BE Carmichael, HJ Glauber, RJ Scully, MO TI Quantum information processing based on cavity QED with mesoscopic systems SO DIRECTIONS IN QUANTUM OPTICS SE Lecture Notes in Physics LA English DT Proceedings Paper CT TAMU-ONR Workshop on Quantum Optics CY JUL 26-30, 1999 CL JACKSON, WY ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; STRONGLY INTERACTING PHOTONS; NONLINEAR CAVITY; COMPUTATION; ENTANGLEMENT; COMMUNICATION; TELEPORTATION; STATES; ATOMS C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. EM mlukin@phase.harvard.edu; mfleisch@mfl.sue.physik.uni-muenchen.de; atac@xanadu.ece.ucsb.edu RI Fleischhauer, Michael/G-6716-2011 NR 36 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0075-8450 BN 3-540-41187-9 J9 LECT NOTES PHYS PY 2001 VL 561 BP 193 EP 203 PG 11 WC Optics; Physics, Applied SC Optics; Physics GA BS55L UT WOS:000170314900018 ER PT J AU Scherneck, HG Johansson, JM Vermeer, M Davis, JL Milne, GA Mitrovica, JX AF Scherneck, HG Johansson, JM Vermeer, M Davis, JL Milne, GA Mitrovica, JX TI BIFROST project: 3-D crustal deformation rates derived from GPS confirm postglacial rebound in Fennoscandia SO EARTH PLANETS AND SPACE LA English DT Article ID GLACIAL ISOSTATIC-ADJUSTMENT; FOCAL MECHANISMS; LEVEL RECORDS; SEA; VLBI; STRESS; EUROPE; MODEL; FIELD; EARTHQUAKES AB Since autumn 1993 the BIFROST project has provided daily GPS solutions of geodetic positions from a network of more than 40 stations covering, a large area of the Baltic shield. This area is expected to show large vertical motion due to glacial isostatic rebound following the deglaciation at the end of the Pleistocene. This paper will discuss the inference of three-dimensional rates of crustal motion at the GPS stations with respect to (1) a plate-fixed average for the horizontal components; (2) a geocentric reference in order to infer absolute changes of sea level from vertical crustal motion and models of geoidal rebound. We show that the horizontal strain rate pattern is largely dominated by unilateral extension and not exhibiting horizontal shear to an important extent. In regard to the vertical motion a crucial issue is the stability of the geocentre in the GPS frame. We show results from an Empirical Orthogonal Function analysis that attenuates regionally correlated noise. In all components our observations suggest reasonably close agreement with forward computions on the basis of postglacial isostatic adjustment. A dominant tectonic signal would lead to a certain fraction of the batch of baselines to exhibit shortening. A tectonic process leading to a similar pattern of horizontal motion as expected from postglacial rebound can safely be dismissed in the context of the currently accepted plate tectonic setting. Thus, our baseline rate comparison will be a critical first order test of the prevailing style of deformation. C1 Chalmers, Onsala Space Observ, SE-43992 Onsala, Sweden. Finnish Geodet Inst, FI-02431 Masala, Finland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02133 USA. Univ Durham, Dept Geol Sci, Durham GH1 3LE, England. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Scherneck, HG (reprint author), Chalmers, Onsala Space Observ, SE-43992 Onsala, Sweden. EM hgs@oso.chalmers.se; mv@fgi.fi; jdavis@cfa.harvard.edu; g.a.milne@durham.ac.uk; jxm@physics.utoronto.ca RI Davis, James/D-8766-2013; Vermeer, Martin/G-2468-2013 OI Davis, James/0000-0003-3057-477X; Vermeer, Martin/0000-0003-3107-6342 NR 52 TC 12 Z9 12 U1 0 U2 5 PU TERRA SCIENTIFIC PUBL CO PI TOKYO PA 2003 SANSEI JIYUGAOKA HAIMU, 5-27-19 OKUSAWA, SETAGAYA-KU, TOKYO, 158-0083, JAPAN SN 1343-8832 J9 EARTH PLANETS SPACE JI Earth Planets Space PY 2001 VL 53 IS 7 BP 703 EP 708 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 464GW UT WOS:000170525700002 ER PT B AU Pawson, DL Ahearn, CA AF Pawson, DL Ahearn, CA BE Barker, M TI Bathyal echinoderms of the Galapagos Islands SO ECHINODERMS 2000 LA English DT Proceedings Paper CT 10th International Echinoderm Conference (IEC) CY JAN 31-FEB 04, 2000 CL UNIV OTAGO, DUNEDIN, NEW ZEALAND HO UNIV OTAGO ID SEA AB Several areas of the Galapagos bathyal, in depths from approximately 105 in to 925 in, were investigated in June-July 1998 using the research submersible Johnson-Sea-Link II. The seabed in the study areas usually consisted of extensive bare rock and patchy soft bottoms ranging from black sand to tan mud. The small collection of echinoderms comprised 27 species, and included four new records for the Galapagos islands and eight new species: four (one representing a new genus), holothurians, one echinoid, and three asteroids. The bathyal echinoderm fauna is characterized by low diversity at the species level and high population densities of a few species. The cidaroid echinoid Centrocidaris doederleini (A.Agassiz), formerly believed to be rare, occurs in numerous populations of one million or more individuals, reaching average densities of 185 individuals per square in. Ophiotrichid and ophiacanthid ophiuroids often occur together in aggregations of more than 100 individuals. Possible benthic feeding behavior of the bathypelagic holothurian Pelagothuria natatrix Ludwig was observed and videotaped. Information on ecology and feeding preferences of approximately 25 species was obtained. Conclusions reached by Maluf (1988,1991) concerning composition and affinities of the Galapagos deepwater echinoderm fauna are supported by the present study. A plea is made for more exploration around Pacific island groups in bathyal/abyssal depths. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Pawson, DL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Mail Stop MRC163, Washington, DC 20560 USA. NR 28 TC 7 Z9 8 U1 0 U2 1 PU A A BALKEMA PUBLISHERS PI LEIDEN PA SCHIPHOLWEG 107C, PO BOX 447, 2316 XC LEIDEN, NETHERLANDS BN 90-5809-189-9 PY 2001 BP 41 EP 46 PG 6 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA BT77P UT WOS:000173978000010 ER PT B AU Lessios, HA AF Lessios, HA BE Barker, M TI Molecular phylogeny of Diadema: Systematic implications SO ECHINODERMS 2000 LA English DT Proceedings Paper CT 10th International Echinoderm Conference (IEC) CY JAN 31-FEB 04, 2000 CL UNIV OTAGO, DUNEDIN, NEW ZEALAND HO UNIV OTAGO ID SPECIES PROBLEM; MASS MORTALITY; PANAMA; ANTILLARUM; ECHINOIDS; PACIFIC; ISTHMUS AB The extreme morphological similarity between species of Diadema has resulted in confused systematics and biogeography. Lessios et al. (in review) constructed a phylogeny based on mitochondrial DNA (mtDNA) from specimens collected around the world. The systematic implications of this phylogeny are discussed here. The molecular data indicate that all Diadema species listed in Mortensen's monograph as valid, except for D. ascensionis, correspond to reciprocally monophyletic mtDNA clades. D. setosum and D. savignyi, far from being subspecies as has been previously suggested, are the most anciently separated extant species of Diadema. There is an undescribed species around the Arabian Peninsula, most closely aligned with D. setosum from the W. Pacific and the Indian Oceans, but quite distinct from it. mtDNA of Diadema in Honshu and Kyushu, Japan does not just belong to D. savignyi or D. setosum, tout also to a separate clade, which could be that of D. clarki, a species described by Ikeda, but dismissed by Mortensen. mtDNA of D. antillarum from the two shores of the Atlantic is as different as mtDNA from D. savignyi, D. paucispinum and D. antillarum. If the latter are maintained as separate species, then D. antillarum should also be split in two. mtDNA of Diadema populations at Ascension and St. Helena forms a monophyletic entity, but one nested within the W. Atlantic clade, supporting Pawson's (1978) demotion of Mortensen's (1909) D. ascensionis to a subspecies of D. antillarum. mtDNA of D. paucispinum is geographically much more widespread than the previously published range of the species, occurring sympatrically with D. savignyi from the central Pacific to the W. Indian Ocean. However, because the two species hybridize, it is riot known whether individuals that contain D. paucispinum mtDNA have D. savignyi nuclear DNA. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Lessios, HA (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 42 TC 5 Z9 5 U1 0 U2 0 PU A A BALKEMA PUBLISHERS PI LEIDEN PA SCHIPHOLWEG 107C, PO BOX 447, 2316 XC LEIDEN, NETHERLANDS BN 90-5809-189-9 PY 2001 BP 487 EP 495 PG 9 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA BT77P UT WOS:000173978000135 ER PT J AU Laurance, WF Perez-Salicrup, D Delamonica, P Fearnside, PM D'Angelo, S Jerozolinski, A Pohl, L Lovejoy, TE AF Laurance, WF Perez-Salicrup, D Delamonica, P Fearnside, PM D'Angelo, S Jerozolinski, A Pohl, L Lovejoy, TE TI Rain forest fragmentation and the structure of Amazonian liana communities SO ECOLOGY LA English DT Article DE Amazon; biomass; edge effects; forest dynamics; habitat fragmentation; liana communities; tree infestation; tropical rainforest; tree mortality; vines ID TIERRA-FIRME FOREST; TREE COMMUNITIES; NATIONAL-PARK; BIOMASS; BRAZIL; DISTURBANCE; MORTALITY; MALAYSIA; DYNAMICS; SARAWAK AB In tropical forests, lianas (woody vines) are important structural parasites of trees. We assessed the effects of forest fragmentation, treefall disturbance, soils, and stand attributes on liana communities in central Amazonian rain forests. Over 27 500 liana stems (greater than or equal to2 cm diameter at breast height [dbh]) were recorded in 27 1-ha plots in continuous forest and 42 plots in 10 forest fragments ranging from 1 to 100 ha in area. For each plot, an index of forest disturbance was determined from a 20-yr study of tree-community dynamics, and 19 soil-texture and chemistry parameters were derived from soil surface samples (top 20 cm). Liana abundance was 187-701 stems/ha, and liana aboveground dry biomass varied from 3.7 to 12.3 Mg/ha. Liana abundance increased significantly near forest edges and was significantly positively associated with forest disturbance and significantly negatively associated with tree biomass. Liana biomass was similarly associated with disturbance and tree biomass but also increased significantly along soil-fertility gradients. Plots near forest edges had a significantly higher proportion of small (2-3 c-m dbh) lianas and relatively fewer large (greater than or equal to4 cm dbh) lianas than did sites in forest interiors. Liana communities were further assessed by comparing their species richness, composition, climbing guilds, and frequency of tree infestation in three 10-ha fragments. Within each fragment, data were collected in 24 small (400-m(2)) plots, with half of the plots near edges and half in interiors. Significantly more trees were infested on fragment edges than in interiors. All three major guilds (branch-twiners, mainstem-twiners, tendril-twiners) were significantly more abundant on edges. Species diversity of lianas (as measured by Fisher's diversity index) also was significantly higher on edges, and this was not simply an artifact of increased liana abundance on edges. We conclude that many aspects of liana community structure are affected by habitat fragmentation, and we suggest that lianas can have important impacts on forest dynamics and functioning in fragmented rain forests. By creating physical stresses on trees and competing for light and nutrients, heavy liana infestations appear partly responsible for the dramatically elevated rates of tree mortality and damage observed near fragment edges. C1 Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. Smithsonian Trop Res Inst, Balboa, Panama. Harvard Univ, Cambridge, MA 02138 USA. Natl Inst Amazonian Res INPA, Dept Ecol, BR-69011970 Manaus, Amazonas, Brazil. Smithsonian Inst, Washington, DC 20560 USA. RP Laurance, WF (reprint author), Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, CP 478, BR-69011970 Manaus, Amazonas, Brazil. RI Laurance, William/B-2709-2012; Fearnside, Philip/D-6559-2011 OI Fearnside, Philip/0000-0003-3672-9082 NR 73 TC 227 Z9 277 U1 11 U2 76 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD JAN PY 2001 VL 82 IS 1 BP 105 EP 116 DI 10.1890/0012-9658(2001)082[0105:RFFATS]2.0.CO;2 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 393UN UT WOS:000166488200009 ER PT J AU Runk, JV AF Runk, JV TI Wounaan and Embera use and management of the fiber palm Astrocaryum standleyanum (Arecaceae) for basketry in eastern Panama SO ECONOMIC BOTANY LA English DT Article DE Astrocaryum standleyanum; Embera; fiber; palm basketry; Panama; Wounaan AB This study examines the use of Astrocaryum standleyanum for basketry by Wounaan and Embera artisans in Panama. Fibers from the palm are a traditional source of material for baskets, which have become commercial art items within the last fifteen years. Data on palm use were collected over two years, largely from Darien Province. Results indicate that the palm is destructively harvested, usually for a single spear leaf. Artisans remove the fibers from the pinnae and color them with dye plants. Astrocaryum standleyanum strands are sewn around a foundation of Carludovica palmata to make coiled baskets. Wounaan weavers are considered the better artisans, perhaps because of cultural traditions or a longer history with art vendors. The sale of A. standleyanum baskets is an important source of cash income, with both domestic and international sales. The destructive harvesting of palms threatens the industry and suggestions are made for sustainable harvest. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Runk, JV (reprint author), Yale Univ, Sch Forestry & Environm Studies, 205 Prospect St, New Haven, CT 06511 USA. NR 36 TC 8 Z9 11 U1 1 U2 7 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 USA SN 0013-0001 J9 ECON BOT JI Econ. Bot. PD JAN-MAR PY 2001 VL 55 IS 1 BP 72 EP 82 DI 10.1007/BF02864547 PG 11 WC Plant Sciences SC Plant Sciences GA 425PK UT WOS:000168300000009 ER PT J AU Joseph, L Slikas, B Alpers, D Schodde, R AF Joseph, L Slikas, B Alpers, D Schodde, R TI Molecular systematics and phylogeography of New Guinean logrunners (Orthonychidae) SO EMU LA English DT Article ID SPECIATION; EVOLUTION; AGES AB The logrunners (Passeriformes: Orthonychidae: Orthonyx) of the montane rainforests of New Guinea are usually treated as conspecific with the Logrunner, Orthonyx temmininckii, of central eastern Australia's upland subtropical rainforests. We used partial mitochondrial DNA (mtDNA.) sequences (cytochrome b and ATPase 8 and 6 genes), largely derived from museum specimens and supplemented with morphometric and plumage data, to re-examine relationships within and among New Guinean and Australian populations of logrunners. The mtDNA sequences from the New Guinean populations are monophyletic and deeply divergent from Australian ones. We cannot with certainty determine whether the sister taxon of the New Guinean populations is the Chowchilla, O. spaldingii, of north-east Queensland's Wet Tropics or O. temminckii. Morphologically, the New Guinean birds are more divergent from Australian O. temminckii than has been appreciated, being significantly smaller and with far less white on their underparts. Their similarities to each other are almost certainly due to retention of ancestral plumage character states. Under any species concept their differences permit the New Guinean birds to be considered as a separate species, O. novaeguineae Meyer, 1874. Within O. novaegidneae, there is a deep phylogeographic break in the distribution of mtDNA diversity between its Vogelkop population in north-western New Guinea and its Snow Mountains and south-eastern highland populations (>5% net nucleotide diversity) in the Central Cordillera. The magnitude of this mtDNA break suggests that, as in endemic birds of the rainforests of north-eastern Queensland, vicariance has operated to fragment these birds' populations at least since the beginning of the Pleistocene if not considerably earlier in the Plio-Miocene. The molecular divergence between Vogelkop and Central Cordillera populations is mirrored in morphology. Weak trends towards birds becoming darker and larger as one moves from west to east across New Guinea may be related to altitude. Taking a cue primarily from the patterns and magnitude of mtDNA divergence, we provisionally recommend taxonomic subdivision of O. novaeguineae. C1 Acad Nat Sci Philadelphia, Dept Ornithol, Philadelphia, PA 19103 USA. Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. Australian Natl Wildlife Collect, CSIRO, Canberra, ACT 2601, Australia. RP Joseph, L (reprint author), Acad Nat Sci Philadelphia, Dept Ornithol, 1900 Benjamin Franklin Pkwy, Philadelphia, PA 19103 USA. RI Joseph, Leo/F-9235-2010; Slikas, Beth/E-7275-2013 NR 36 TC 21 Z9 21 U1 1 U2 3 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 0158-4197 J9 EMU JI Emu PY 2001 VL 101 IS 4 BP 273 EP 280 DI 10.1071/MU01008 PG 8 WC Ornithology SC Zoology GA 509MJ UT WOS:000173151300001 ER PT J AU Christen, CA AF Christen, CA TI Parks in peril: People, politics, and protected areas. SO ENVIRONMENTAL HISTORY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Christen, CA (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 2 PU ENVIRONMENTAL HISTORY PI DURHAM PA 701 VICKERS AVE, DURHAM, NC 27701-3147 USA SN 1084-5453 J9 ENVIRON HIST JI Environ. Hist. PD JAN PY 2001 VL 6 IS 1 BP 137 EP 139 DI 10.2307/3985247 PG 3 WC Environmental Studies; History SC Environmental Sciences & Ecology; History GA 396JB UT WOS:000166631600018 ER PT B AU Lobel, A AF Lobel, A BE Gull, TR Johansson, S Davidson, K TI Spatially resolved STIS spectroscopy of Betelgeuse: Evidence for non-radial chromospheric oscillation from detailed modeling SO ETA CARINAE AND OTHER MYSTERIOUS STARS: THE HIDDEN OPPORTUNITIES OF EMISSION LINE SPECTROSCOPY SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT International Conference on ETA Carinae and Other Mysterious Stars CY AUG 24-26, 2000 CL HVEN, SWEDEN SP Royal Swedish Acad Sci, Crafoord Fdn, Royal Physiog Soc AB A spectral analysis of Betelgeuse (M2 Iab), a cool peculiar emission line supergiant is presented. Four spatially resolved raster scans across the chromospheric disk have been obtained with the STIS (HST) between 1998 January and 1999 March. These near-UV spectra display many double-peaked permitted emission lines of neutral and singly ionized metals with self-absorbed cores. In 1998 September we observe a reversal in the intensity of both emission line components when scanning across the disk, for four unsaturated lines of Si I (UV 1), Fe II (UV 61), Al II (UV 1), and Fe II (UV 36). The Si I lambdalambda2516 resonance line is modeled with detailed radiative transport calculations in spherical geometry, and a mean velocity structure in the chromospheric projected area is constrained for each aperture position on the UV disk. The spatial radial velocity structure of Betelgeuse's chromosphere reveals opposite flow velocities of similar to2 kms(-1) in 1998 September. These sub-sonic velocities indicate non-radial (or non-coherent) movements in the lower chromosphere during certain phases of the stellar pulsation cycle. This observation may provide important clues on the prevalent mass-loss mechanism of cool massive stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lobel, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-080-3 J9 ASTR SOC P PY 2001 VL 242 BP 241 EP 246 PG 6 WC Astronomy & Astrophysics; Spectroscopy SC Astronomy & Astrophysics; Spectroscopy GA BU31W UT WOS:000175679300033 ER PT J AU Disney, RHL Sakai, S AF Disney, RHL Sakai, S TI Scuttle flies (Diptera : Phoridae) whose larvae develop in flowers of Aristolochia (Aristolochiaceae) in Panama SO EUROPEAN JOURNAL OF ENTOMOLOGY LA English DT Article DE Diptera; Phoridae; new species; new synonymy; new combinations; Aristolochiaceae; Neotropical Region AB Megaselia metropolitanoensis Disney, sp. n., M sakaiae Disney, sp. n. and Puliciphora pygmaea (Borgmeier, 1960) comb. n. are reported developing in the flowers of Aristolochia inflata H. B. K. and A. maxima Jacq. in Panama. The new species are described, as is the hitherto unknown male of Puliciphora pygmaea. The latter is transferred to the the genus Puliciphora Dahl, 1897 from the genus Myrmomyia Silvestri, 1911 which is formally synonymised with Puliciphora, along with P. brachymyrmecis (Silvestri, 1911) comb. n. and P. nigroflava (Borgmeier, 1958) comb. n. C1 Univ Cambridge, Museum Zool, Cambridge CB2 3EJ, England. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Disney, RHL (reprint author), Univ Cambridge, Museum Zool, Downing St, Cambridge CB2 3EJ, England. NR 20 TC 10 Z9 15 U1 0 U2 0 PU CZECH ACAD SCI, INST ENTOMOLOGY PI CESKE BUDEJOVICE PA BRANISOVSKA 31, CESKE BUDEJOVICE 370 05, CZECH REPUBLIC SN 1210-5759 J9 EUR J ENTOMOL JI Eur. J. Entomol. PY 2001 VL 98 IS 3 BP 367 EP 373 PG 7 WC Entomology SC Entomology GA 497KW UT WOS:000172455400011 ER PT J AU Eberhard, WG AF Eberhard, WG TI Species-specific genitalic copulatory courtship in sepsid flies (Diptera, Sepsidae, Microsepsis) and theories of genitalic evolution SO EVOLUTION LA English DT Article DE copulatory courtship; cryptic female choice; genitalic evolution; sexual selection ID SEXUAL SELECTION; MATING-BEHAVIOR AB Males of Microsepsis eberhardi and M. armillata use their genitalic surstyli to rhythmically squeeze the female's abdomen with stereotyped movements during copulation. Squeezing movements did not begin until intromission had occurred and, contrary to predictions of the conflict-of-interest hypothesis for genitalic evolution, did not overcome morphological or behavioral female resistance. Contrary to predictions of the lock-and-key hypothesis, female morphology was uniform in the two species and could not mechanically exclude the genitalia of either species of male. The complex pattern of squeezing movements differed between the two species as predicted by the sexual selection hypothesis for genitalic evolution. Also, evolutionarily derived muscles and pseudoarticulations in the male's genitalic surstyli facilitated one type of movement, whose patterns were especially distinct. The data support the hypothesis that the male surstyli evolved to function as courtship devices. C1 Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, San Jose, Costa Rica. NR 31 TC 61 Z9 63 U1 0 U2 15 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD JAN PY 2001 VL 55 IS 1 BP 93 EP 102 PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 405NY UT WOS:000167167000008 PM 11263749 ER PT B AU Kalogera, V AF Kalogera, V BE Podsiadlowski, P Rappaport, S King, A DAntona, F Burderi, L TI The formation of black-hole X-ray transients SO EVOLUTION OF BINARY AND MULTIPLE STAR SYSTEMS: A MEETING IN CELEBRATION OF PETER EGGLETON'S 60TH BIRTHDAY SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Evolution of Binary and Multiple Star Systems CY JUN 25-JUL 01, 2000 CL BORMIO, ITALY SP Osservatorio Astronomico Roma, Lawrence Livermore Natl Lab ID MASS; EVOLUTION; BINARIES; STARS AB Studies of the observed characteristics of black-hole (BH) X-ray binaries can provide us with valuable information about the process of BH formation. In this paper I address some of the aspects of our current understanding of BH formation in binaries and point out some of the existing problems of current theoretical models. In particular, the measured orbital periods and donor-star properties indicate that a common-envelope phase appears to be a necessary ingredient of the evolutionary history of observed BH X-ray transients, and that it must be associated only with a modest orbital contraction. The timing of this common-envelope phase is crucial in determining the final BH masses and current evolutionary models of mass-losing massive stars place strong constraints on the possible masses for immediate BH progenitors and wind mass loss from helium stars. Last, it is interesting that, even in the absence of any source of mass loss, the highest helium-star masses predicted by current evolutionary models are still not high enough to account for the measured BH mass in V404 Cyg (> 10 Mcircle dot). An alternative for the formation of relatively massive BH may be provided by the evolutionary sequence proposed by Eggleton & Verbunt (1986), which invokes hierarchical triples as progenitors of BH X-ray binaries with low-mass companions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kalogera, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 19 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-061-7 J9 ASTR SOC P PY 2001 VL 229 BP 537 EP 546 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU52C UT WOS:000176235800061 ER PT S AU Vaisanen, P Tollestrup, EV Willner, SP Cohen, M AF Vaisanen, P Tollestrup, EV Willner, SP Cohen, M BE Harwit, M Hauser, MG TI New wide field J- and K-band galaxy counts and the extragalactic background SO EXTRAGALACTIC INFRARED BACKGROUND AND ITS COSMOLOGICAL IMPLICATIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union C1 Univ Helsinki Observ, Helsinki 00014, Finland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. RP Vaisanen, P (reprint author), Univ Helsinki Observ, Helsinki 00014, Finland. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-062-5 J9 IAU SYMP PY 2001 IS 204 BP 215 EP 216 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU43Y UT WOS:000175997600028 ER PT J AU Winter, K Garcia, M Gottsberger, R Popp, M AF Winter, K Garcia, M Gottsberger, R Popp, M TI Marked growth response of communities of two tropical tree species to elevated CO2 when soil nutrient limitation is removed SO FLORA LA English DT Article DE CO2 exchange; elevated CO2; growth; nutrients; trees; tropical forest ID ATMOSPHERIC CO2; CARBON-DIOXIDE; PLANT-GROWTH; PHOTOSYNTHESIS; SEEDLINGS; PHYSIOLOGY; ENRICHMENT; ECOSYSTEMS; FORESTS; AMBIENT AB As part of an ongoing project to understand the effects of elevated atmospheric CO2 on plants in complex, tropical communities, we studied biomass accumulation in a simplified model seedling community consisting of two species of tropical trees (Ficus insipida, a fast growing pioneer species, and Virola surinamensis, a slow-growing, shade-tolerant late successional species). The plants were grown at ambient and elevated (about two times ambient) CO2 concentrations using open-top chambers at a field site in Panama. Communities grew in heavily fertilized soil. Compared to a previous experiment with model communities of F. insipia and V. surinamensis grown on unfertilized soil (WINTER et al., Flora [2000] 195, 289) application of soil fertilizer markedly accelerated community growth rates at ambient CO2, and biomass accumulation was enhanced by an additional 52% at elevated CO2. In contrast, elevated CO2 had no significant effect on biomass accumulation in unfertilized communities. Communities growing on fertilized soil showed greater biomass allocation into leaves, i.e. higher leaf weight ratios (LWRs) than did communities on unfertilized soil. Higher LWRs were related to lower root: shoot ratios and together with greater specific leaf areas (area per unit leaf mass), largely a consequence of lower leaf starch contents, resulted in higher leaf area ratios (LARs). While elevated CO2 caused the relatively low LARs in unfertilized communities to decrease further, by strongly increasing leaf starch levels and decreasing specific leaf areas, these leaf characteristics changed only slightly in fertilized communities exposed to elevated CO2. Thus, by maintaining relatively high LARs at elevated CO2, fertilized plants were able to effectively use enhanced CO2 concentrations for increased carbon gain and growth. Leaves of plants on fertilized soil were characterized by relatively low C:N ratios which were largely unaffected by CO2 concentration. In contrast, C:N ratios in leaves of unfertilized plants were higher than those of fertilized plants and increased in response to elevated CO2. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Vienna, Inst Pflanzenphysiol, A-1091 Vienna, Austria. RP Winter, K (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. RI Popp, Marianne/E-7559-2012 NR 36 TC 19 Z9 20 U1 2 U2 12 PU URBAN & FISCHER VERLAG PI JENA PA BRANCH OFFICE JENA, P O BOX 100537, D-07705 JENA, GERMANY SN 0367-2530 J9 FLORA JI Flora PY 2001 VL 196 IS 1 BP 47 EP 58 PG 12 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 415DB UT WOS:000167704500003 ER PT J AU Stuntz, S Zotz, G AF Stuntz, S Zotz, G TI Photosynthesis in vascular epiphytes: A survey of 27 species of diverse taxonomic origin SO FLORA LA English DT Article DE vascular epiphytes; BCI; leaf nitrogen; O-2 electrode; photosynthesis; PNUE ID CRASSULACEAN ACID METABOLISM; NITROGEN-USE EFFICIENCY; GUZMANIA-MONOSTACHIA; COMPARATIVE ECOPHYSIOLOGY; RESPIRATORY CO2; C-3 BROMELIADS; CARBON BALANCE; WATER-STRESS; GAS-EXCHANGE; CAM PLANTS AB Light-saturation curves of photosynthetic oxygen evolution were determined for a set of 27 species of vascular epiphytes, naturally growing in the moist tropical lowland forest of Barro Colorado Island, Panama. Leaf samples were selected fi om species in eight growing families, mostly from members of the Orchidaceae, Bromeliaceae, Araceae, and fi am two fern families, the Polypodiaceae and Vittariaceae. Growing sites covered all strata of the forest. Photosynthetic characteristics of this diverse species assemblage covered a wide range. with several species exhibiting considerably higher net photosynthetic capacities (PC) than previously reported for vascular epiphytes : the maximum PC, in the orchid Caularthron bilamellatum, was c. 40 mu mol O-2 m(-2) s(-1). As expected, PC was a function of leaf nitrogen content. Physiological characteristics con elated well with the growing site within the forest, while taxonomic groups did not vary in leaf physiological parameters, with one exception: the photosynthetic nitrogen use efficiency (PNUE) differed significantly between bromeliads, orchids and aroids, being highest in the first and lowest in the latter family. C1 Univ Wurzburg, Lehrstuhl Bot 2, D-8700 Wurzburg, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Zotz, G (reprint author), Univ Basel, Inst Bot, Schonbeinstr 6, CH-4056 Basel, Switzerland. NR 53 TC 24 Z9 25 U1 5 U2 18 PU URBAN & FISCHER VERLAG PI JENA PA BRANCH OFFICE JENA, P O BOX 100537, D-07705 JENA, GERMANY SN 0367-2530 J9 FLORA JI Flora PY 2001 VL 196 IS 2 BP 132 EP 141 PG 10 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 432PJ UT WOS:000168701900005 ER PT J AU Winter, K Aranda, J Garcia, M Virgo, A Paton, SR AF Winter, K Aranda, J Garcia, M Virgo, A Paton, SR TI Effect of elevated CO2 and soil fertilization on whole-plant growth and water use in seedlings of a tropical pioneer tree, Ficus insipida Willd. SO FLORA LA English DT Article DE atmospheric CO2; Ficus insipida; global change; growth; tropical forest; water use ID ATMOSPHERIC CO2; USE EFFICIENCY; DRYING SOIL; FOREST; PHOTOSYNTHESIS; TRANSPIRATION; RESPONSES; NITROGEN; PRODUCTIVITY; WET AB Seedlings of the tropical pioneer tree species Ficus insipida were cultivated at present-ambient and elevated (about twice-ambient) CO2 concentrations in open-top chambers located in a forest clearing near Panama City, Republic of Panama. To examine potential chamber-specific effects on growth and transpiration, plants were also studied outside chambers at ambient CO2 levels. Plants were grown individually in 38 litre pots containing a mixture of soil and leaf litter, either in the absence or presence of a slow-release fertilizer. Data from three experiments. lasting 7 to 9 weeks each, are presented. Transpirational water loss of plants was determined gravimetrically. Fertilized plants grew more rapidly than unfertilized plants. Elevated CO2 strongly enhanced biomass accumulation in fertilized plants. In unfertilized plants, elevated CO2 enhanced growth in two experiments, but not in a third. Transpiration ratios (TR, g water lost: g dry mass accumulated) of plants grown in open-top chambers ranged from 176 (elevated CO2 plus fertilizer) to 336 (ambient CO2, minus fertilizer). The addition of fertilizer decreased TR by 15 to 20%, irrespective of the CO2 concentration, and elevated CO2 reduced TR by 27 to 35%, irrespective of whether fertilizer was present or not. The reduction in TR in response to elevated CO2, was independent of whether biomass accumulation was enhanced by elevated CO2 or not. In all experiments in which biomass accumulation was increased at elevated CO2, absolute water expenditure at elevated CO2 was greater or similar to that at ambient levels - despite the lower TR at elevated CO2 In the single experiment in which elevated CO2 diet not lead to increased growth, the absolute water expenditure of plants was lower at elevated than at ambient CO2. There was no chamber effect on biomass accumulation, but TR of both fertilized and unfertilized plants was 19 to 31% higher inside compared to outside the open-top chambers. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Winter, K (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Ancon, Panama. NR 27 TC 20 Z9 21 U1 1 U2 9 PU URBAN & FISCHER VERLAG PI JENA PA BRANCH OFFICE JENA, P O BOX 100537, D-07705 JENA, GERMANY SN 0367-2530 J9 FLORA JI Flora PY 2001 VL 196 IS 6 BP 458 EP 464 PG 7 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 503DN UT WOS:000172782900004 ER PT S AU Guenther, EW Joergens, V Neuhauser, R Torres, G Batalha, NS Vijapurkar, J Fernandez, M Mundt, R AF Guenther, EW Joergens, V Neuhauser, R Torres, G Batalha, NS Vijapurkar, J Fernandez, M Mundt, R BE Zinnecker, H TI A spectroscopic and photometric survey for pre-main sequence binaries SO FORMATION OF BINARY STARS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 200th Symposium of the International-Astronomical-Union CY APR 10-15, 2000 CL ASTROPHYS INST POTSDAM, POTSDAM, GERMANY SP Int Astron Union HO ASTROPHYS INST POTSDAM AB We give here an overview of the current state of our survey for pro-main sequence spectroscopic binaries. Up to now we have taken 739 spectra of 250 pre-main sequence stars. We find that 8% of the stars show significant radial velocity variations, and are thus most likely spectroscopic binaries. In addition to the targets showing radial velocity variations, 6% of the targets are double-lined spectroscopic binaries i.e., the total fraction of spectroscopic binaries is expected to be about 14%. All short-period SB2s are monitored photometrically in order to search for eclipses. An eclipsing SB2 would allow the direct measurement of the masses of both stellar components. Measurements of the stellar masses together with determinations of the stellar radii are a crucial test of evolutionary tracks of pre-main sequence stars. C1 Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. MPI Extraterr Phys, D-85740 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, Ames Res Ctr, Planetary Syst Branch, Moffett Field, CA 94035 USA. Homi Bhabha Ctr Sci Educ, Mumbai, India. Inst Astrofis Andalucia, E-18080 Granada, Spain. MPI Astron, D-69117 Heidelberg, Germany. RP Guenther, EW (reprint author), Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. NR 4 TC 0 Z9 0 U1 0 U2 2 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-068-4 J9 IAU SYMP PY 2001 IS 200 BP 165 EP 168 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU43W UT WOS:000175996700020 ER PT S AU Kenyon, SJ Hartigan, P AF Kenyon, SJ Hartigan, P BE Zinnecker, H TI First results from a STIS survey of close pre-main sequence binaries in Taurus SO FORMATION OF BINARY STARS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 200th Symposium of the International-Astronomical-Union CY APR 10-15, 2000 CL ASTROPHYS INST POTSDAM, POTSDAM, GERMANY SP Int Astron Union HO ASTROPHYS INST POTSDAM ID ORION-NEBULA; STARS; ACCRETION; DISK; EMISSION; SCORPIUS; AURIGA AB We describe preliminary results of an HST survey of premain sequence binary stars in the Taurus-Auriga cloud. We use STIS medium and low resolution spectra to derive the reddening, spectral type, and veiling for each component of close pairs with angular separations less than or equal to 1". This sample yields a frequency of mixed pairs, containing one classical and one weak emission T Tauri star, similar to that of wide pre-main sequence binaries. The components of most pairs are coeval, but the secondaries in four pairs are significantly younger than the primaries for the three sets of evolutionary tracks we considered. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, Mail Stop 15,60 Garden St, Cambridge, MA 02138 USA. NR 30 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-068-4 J9 IAU SYMP PY 2001 IS 200 BP 323 EP 331 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU43W UT WOS:000175996700039 ER PT S AU Di Stefano, R AF Di Stefano, R BE Zinnecker, H TI Microlensing: A tool to probe distant binary populations SO FORMATION OF BINARY STARS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 200th Symposium of the International-Astronomical-Union CY APR 10-15, 2000 CL ASTROPHYS INST POTSDAM, POTSDAM, GERMANY SP Int Astron Union HO ASTROPHYS INST POTSDAM ID GRAVITATIONAL LENSING EXPERIMENT; VARIABLE-STARS; PLANETARY SYSTEMS; GLOBULAR-CLUSTERS; OMEGA-CENTAURI; MACHO PROJECT; CCD SEARCH; EVENTS AB Programs designed to observe gravitational microlensing are poised to provide a great deal of information about binary populations far from Earth, including those in the Galactic Bulge, in the Magellanic Clouds, in M31, and perhaps in other external galaxies. Because many millions of stars are monitored, microlensing observations allow us to study binaries in three ways: (1) when they are "involved" in a microlensing event (as either a lens or lensed source), (2) when variability due to binarity produces significant variations in the light curve, and (3) when light from a more distant star is attenuated or refracted by matter associated with the binary system (e.g., in a disk). Microlensing observations will discover large numbers of binaries and planetary systems in a variety of galactic environments. Thus, comparative statistical studies of binary properties (distributions of mass ratios and orbital separations) are possible. An intriguing sign that we have already begun to learn about binaries through microlensing observations comes from work indicating that all of the lenses detected to date may in fact be binaries. For observations along the direction of the Magellanic Clouds this would imply that, if the lenses are primarily located in the Halo, then MACHOs tend to be binaries. If, on the other hand, most of the lenses are located in the Magellanic Clouds, microlensing observations are giving us a unique way to explore a distant stellar population of binaries. C1 Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Di Stefano, R (reprint author), Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. NR 23 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-068-4 J9 IAU SYMP PY 2001 IS 200 BP 529 EP 538 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU43W UT WOS:000175996700066 ER PT B AU Myers, PC AF Myers, PC BE Montmerle, T Andre, P TI Cluster formation in turbulent dense cores SO FROM DARKNESS TO LIGHT: ORIGIN AND EVOLUTION OF YOUNG STELLAR CLUSTERS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 3rd 3-Island European Conference on Stellar Clusters and Associations - From Darkness to Light CY APR 03-08, 2000 CL CARGESE, FRANCE SP European Comm DE ISM : turbulence; cores : formation, cluster-forming, kernels; stars : IMF; regions : serpens, perseus, OMC2/3; instruments : BIMA, IRAM-PdBI; OVRO ID INITIAL MASS FUNCTION; STAR-FORMATION; BROWN DWARFS; DARK CLOUDS AB Observations of nearby cluster-forming regions indicate numerous condensations which have a separations and masses similar to those of embedded stars, and which are local minima of turbulent motions. We present high-resolution observations of these condensations in Serpens, Perseus, Orion, and Ophiuchus. These objects are good candidates to form the next "generation" of cluster stars. We present a simple model of cluster formation based on these observations, in which condensations form via dissipation of turbulence, and grow by accretion. The growth can be interrupted by fragmentation or terminated by star-forming collapse. Such a model can form stars whose mass distribution reproduces the main features of the IMF, in times of order 1 Myr. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Myers, PC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 42, Cambridge, MA 02138 USA. NR 27 TC 5 Z9 5 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-081-1 J9 ASTR SOC P PY 2001 VL 243 BP 131 EP 138 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU34A UT WOS:000175724100012 ER PT B AU Padoan, P Nordlund, A Rognvaldsson, OE Goodman, A AF Padoan, P Nordlund, A Rognvaldsson, OE Goodman, A BE Montmerle, T Andre, P TI Turbulent fragmentation and the initial conditions for star formation SO FROM DARKNESS TO LIGHT: ORIGIN AND EVOLUTION OF YOUNG STELLAR CLUSTERS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 3rd 3-Island European Conference on Stellar Clusters and Associations - From Darkness to Light CY APR 03-08, 2000 CL CARGESE, FRANCE SP European Comm DE ISM : clouds, dynamics, turbulence, magnetic fields; cores : mass distribution; stars : formation, IMF ID MOLECULAR CLOUDS; DENSE CORES; DARK CLOUDS; HIERARCHICAL STRUCTURE; ENERGY-DISSIPATION; MAGNETIC CLOUDS; JEANS COLLAPSE; EVOLUTION; FIELD; MODEL AB Supersonic turbulence fragments molecular clouds (MC) into a very complex density field with density contrasts of several orders of magnitude. A fraction of the gas is locked into dense and gravitationally bound cores, which collapse as proto stars. This process can be studied with numerical simulations of super-sonic self-gravitating turbulence. In this work, we use numerical simulations of magneto-hydrodynamic (MHD), super-sonic, super-Alfvenic and self-gravitating turbulence to compute the mass distribution of collapsing proto-stellar cores, which are selected as local density maxima. We find that the mass distribution of collapsing cores is consistent with the stellar initial mass function (IMF), suggesting that turbulence alone might be responsible for the generation of the IMF. To support this conclusion we also show that the physical properties of the numerically selected cores are in agreement with the properties of observed NH3 cores and that their magnetic field strength is consistent with Zeeman splitting measurements. In turbulent MCs, star formation occurs via the gravitational collapse of super-critical cores, formed by the turbulent flow, sub-critical cores being irrelevant for the process of star formation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Padoan, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 42 TC 7 Z9 7 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-081-1 J9 ASTR SOC P PY 2001 VL 243 BP 279 EP 290 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU34A UT WOS:000175724100025 ER PT B AU Harnden, FR Murray, SS Wolk, SJ Damiani, F Flaccomio, E Micela, G Pizzolato, N Sciortino, S AF Harnden, FR Murray, SS Wolk, SJ Damiani, F Flaccomio, E Micela, G Pizzolato, N Sciortino, S BE Montmerle, T Andre, P TI The Chandra HRC image of the orion trapezium region SO FROM DARKNESS TO LIGHT: ORIGIN AND EVOLUTION OF YOUNG STELLAR CLUSTERS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 3rd 3-Island European Conference on Stellar Clusters and Associations - From Darkness to Light CY APR 03-08, 2000 CL CARGESE, FRANCE SP European Comm DE clusters : OB associations; stars : X-rays, coronae; X-rays : stars; regions : ONC, trapezium instruments : Chandra AB We present results of a 63 ksec Chandra HRC-I observation of the Orion Trapezium region. We have detected nearly 800 distinct sources most of which are associated with known Orion Nebula Cluster members. The superb angular resolution of the Clandra mirrors frees our analysis from the source confusion problems that have plagued previous investigations of the X-ray emission of this fascinating region and allows us to explore the relationship between X-ray emission levels and other stellar parameters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harnden, FR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-081-1 J9 ASTR SOC P PY 2001 VL 243 BP 461 EP 464 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU34A UT WOS:000175724100044 ER PT B AU Luhman, KL Rieke, GH AF Luhman, KL Rieke, GH BE Montmerle, T Andre, P TI The initial mass function of low-mass stars and brown dwarfs SO FROM DARKNESS TO LIGHT: ORIGIN AND EVOLUTION OF YOUNG STELLAR CLUSTERS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 3rd 3-Island European Conference on Stellar Clusters and Associations - From Darkness to Light CY APR 03-08, 2000 CL CARGESE, FRANCE SP European Comm DE stars : low-mass, PMS evolution, formation, brown dwarfs, IMF; regions : tapezium, IC 348, rho Oph, Taurus, Pleiades; instruments : HST, 2MASS ID MOLECULAR CLOUDS; YOUNG CLUSTERS; SPECTRUM; TAURUS AB We present measurements of the Initial Mass Function (IMF) that are complete to 0.01-0.02 M-circle dot for the star forming clusters of the Trapezium, IC 348, and Ophiuchus and the region of more isolated star formation in Taurus. The mass functions of the three clusters, Taurus, the Pleiades open cluster, the field, globular clusters, and pre-stellar clumps are compared. We test the predictions of theories of the IMF against these data. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 31 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-081-1 J9 ASTR SOC P PY 2001 VL 243 BP 493 EP 498 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU34A UT WOS:000175724100049 ER PT B AU Wolk, SJ Cover, RT Jayawardhana, R Hearty, TJ AF Wolk, SJ Cover, RT Jayawardhana, R Hearty, TJ BE Montmerle, T Andre, P TI MBM 12: A younger version of the TW hydrae association? SO FROM DARKNESS TO LIGHT: ORIGIN AND EVOLUTION OF YOUNG STELLAR CLUSTERS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 3rd 3-Island European Conference on Stellar Clusters and Associations - From Darkness to Light CY APR 03-08, 2000 CL CARGESE, FRANCE SP European Comm DE pre-main sequence, low-mass, X-rays; MBM 12, TW Hya; instruments : 2MASS, Whipple, Hipparcos ID STARS AB We present optical and infrared photometry of stars near the MBM 12 dart; cloud. The optical data indicate that there are about 40 candidate pre-main sequence stars in the same area currently occupied by eight bona-fide PMS stars. Analysis of 2MASS data suggests that 60% of PMS candidates had been detected. Some of these show evidence of optically thick disks. Our study of the 2MASS data also reveals a large enhancement of sources within the MBM 12 cloud, indicating that it is still actively forming stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-081-1 J9 ASTR SOC P PY 2001 VL 243 BP 687 EP 692 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU34A UT WOS:000175724100071 ER PT S AU Garcia, MR Murray, SS Primini, FA Forman, WR Jones, C McClintock, JE AF Garcia, MR Murray, SS Primini, FA Forman, WR Jones, C McClintock, JE BE Schilizzi, RT Vogel, SN Paresce, F Elvis, MS TI Chandra observations of M31 SO GALAXIES AND THEIR CONSTITUENTS AT THE HIGHEST ANGULAR RESOLUTIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union ID REGION AB As part of the Chandra GTO program we are monitoring and surveying M31 using the HRC and ACIS cameras. These observations have-resolved the nuclear X-ray source into five separate sources, one of which is very soft and may (or may not!) be associated with the central super-massive black hole. In addition, the superb spatial resolution and low scattering of the Chandra telescope allows us to unambiguously resolve the diffuse emission from the point sources. This emission is clearly softer than the point sources, and also increases with temperature radially. The monitoring nature of the observations allows detailed study of the variability of the point sources. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Garcia, MR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 NR 15 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-066-8 J9 IAU SYMP PY 2001 IS 205 BP 38 EP 41 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU43Z UT WOS:000175998000008 ER PT S AU Karovska, M Aldcroft, T Elvis, MS Evans, IN Fabbiano, G Gaetz, TJ Isobe, T Jerius, D Jones, C Juda, M Kenter, A Kim, DW Kraft, RP Murray, SS Prestwich, AH Primini, F Schwartz, DA Cui, W Schreier, EJ AF Karovska, M Aldcroft, T Elvis, MS Evans, IN Fabbiano, G Gaetz, TJ Isobe, T Jerius, D Jones, C Juda, M Kenter, A Kim, DW Kraft, RP Murray, SS Prestwich, AH Primini, F Schwartz, DA Cui, W Schreier, EJ BE Schilizzi, RT Vogel, SN Paresce, F Elvis, MS TI Deconvolving the nucleus of centaurus using a Chandra PSF library SO GALAXIES AND THEIR CONSTITUENTS AT THE HIGHEST ANGULAR RESOLUTIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union ID IMAGE AB We describe preliminary results from our study of multi-scale structures in Centaurus A (NGC 5128) obtained using the Chandra X-ray Observatory HRC-I observations. The high-angular resolution Chandra images reveal X-ray multi-scale structures in this object with unprecedented detail and clarity. The region surrounding the Cen A nucleus, believed to be associated with a supermassive black hole, shows structures on arcsecond scales clearly resolved from the central source. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Purdue Univ, W Lafayette, IN 47907 USA. RP Karovska, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-066-8 J9 IAU SYMP PY 2001 IS 205 BP 66 EP 69 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU43Z UT WOS:000175998000016 ER PT S AU Brunthaler, A Falcke, H Bower, GC Aller, M Aller, H Terasranta, H AF Brunthaler, A Falcke, H Bower, GC Aller, M Aller, H Terasranta, H BE Schilizzi, RT Vogel, SN Paresce, F Elvis, MS TI III Zw 2: Superluminal motion and compact lobe expansion in a Seyfert galaxy SO GALAXIES AND THEIR CONSTITUENTS AT THE HIGHEST ANGULAR RESOLUTIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union ID QUASARS; RADIO AB So far all relativistically boosted jets with superluminal motion have only been detected in normal radio galaxies that have early-type host galaxies. We have now discovered superluminal motion in the Seyfert 1 galaxy III Zw 2, classified as a spiral. Spectral and spatial evolution axe closely linked. Since III Zw 2 is part of a sample of so-called radio-intermediate quasars (RIQ), it confirms earlier predictions of superluminal motion for this source, based on the argument that RIQs could be relativistically boosted jets in radio-weak quasars and Seyfert galaxies. C1 Max Planck Inst Radioastron, D-5300 Bonn, Germany. Natl Radio Astron Observ, Socorro, NM 87801 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Metsahovi Radiol Res Stn, Kylmala, Finland. Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brunthaler, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-5300 Bonn, Germany. RI Falcke, Heino/H-5262-2012 OI Falcke, Heino/0000-0002-2526-6724 NR 3 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-066-8 J9 IAU SYMP PY 2001 IS 205 BP 110 EP 111 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU43Z UT WOS:000175998000034 ER PT S AU Fabbiano, G AF Fabbiano, G BE Schilizzi, RT Vogel, SN Paresce, F Elvis, MS TI Chandra observations of the antennae galaxies (NGC 4038/39) SO GALAXIES AND THEIR CONSTITUENTS AT THE HIGHEST ANGULAR RESOLUTIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union AB A deep (similar to 70ks) Chandra ACIS pointing at the merging system NGC 4038/39 gives us an exceptional detailed view of its X-ray emission and demonstrates the capabilities of Chandra's sub-arcsecond resolution. We detect an extraordinarily luminous population of point-like sources, that may suggest 10 - 100M(circle dot) Black Hole counterparts. We also detect a luminous hot ISM, with features ranging to large scale outflows to hot superbubbles. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-066-8 J9 IAU SYMP PY 2001 IS 205 BP 202 EP 205 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU43Z UT WOS:000175998000069 ER PT S AU Prestwich, A Zezas, A Kaaret, P Murray, S Kilgard, R Kim, DW Schlegel, E Ward, M Lira, P AF Prestwich, A Zezas, A Kaaret, P Murray, S Kilgard, R Kim, DW Schlegel, E Ward, M Lira, P BE Schilizzi, RT Vogel, SN Paresce, F Elvis, MS TI Chandra observations of starburst galaxies M82 and NGC 3256 SO GALAXIES AND THEIR CONSTITUENTS AT THE HIGHEST ANGULAR RESOLUTIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union ID EMISSION AB We present high resolution Chandra X-ray imaging of two starburst galaxies, M82 and NGC 3256. The central x-ray source observed by ROSAT and ASCA in M82 is resolved into 3 or 4 sources. Most of these sources are variable, suggesting that the point sources axe powered by accretion. The brightest of these central sources is similar to 10(41) ergs s(-1) in the high state, and is responsible for the variability observed by ROSAT and ASCA. Assuming this source radiates at the Eddington limit, the mass is similar to 500M(circle dot). The diffuse hard (2-10 keV) emission in M82 is spatially coincident with diffuse radio emission and Palpha. This is consistent with diffuse hard X-ray emission arising from hot thermal gas in the starburst region. Approximately 14 sources with L-x > 10(39) ergs s(-1) were detected in NGC 3256, including both nuclei. Two of these sources have L-x > 10(40) ergs s(-1). This observation suggests that "super Edington" sources may be preferentially associated with starburst galaxies (see also paper by Fabbiano in this volume). C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Prestwich, A (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 8 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-066-8 J9 IAU SYMP PY 2001 IS 205 BP 208 EP 211 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU43Z UT WOS:000175998000071 ER PT S AU Lebach, DE Ratner, MI Shapiro, II Ransom, RR Bartel, N Bietenholz, MF Lestrade, JF AF Lebach, DE Ratner, MI Shapiro, II Ransom, RR Bartel, N Bietenholz, MF Lestrade, JF BE Schilizzi, RT Vogel, SN Paresce, F Elvis, MS TI VLBI Imaging and astrometry of the RS CVn binary star IM Pegasi SO GALAXIES AND THEIR CONSTITUENTS AT THE HIGHEST ANGULAR RESOLUTIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union ID RADIO AB We have made 3.6 cm VLBI observations of the RS CVn binary star IM Pegasi (HR 8703) approximately four times per year since 1997 in support of the NASA/Stanford Relativity Gyroscope Experiment (Gravity Probe B). Phase-referenced maps reveal structural changes in the radio emission of the star on hour time scales during several of the sessions. Analyses of the VLBI phase delays with a Kalman-filter estimator reveal submilliarcsecond motions of the radio centroid of the star on hour and even subhour time scales. The observed structural changes and centroid motions often coincide with rapid changes in the star's flux density, as measured with the VLA. We report on our latest results and summarize our findings to date. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. York Univ, Dept Phys & Astron, N York, ON M3J 1P3, Canada. Observ Paris, F-92195 Meudon, France. RP Lebach, DE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-066-8 J9 IAU SYMP PY 2001 IS 205 BP 318 EP 321 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU43Z UT WOS:000175998000107 ER PT S AU Greenhill, LJ Moran, JM Booth, RS Ellingsen, SP McCulloch, PM Jauncey, DL Norris, RP Reynolds, JE Tzioumis, AX Herrnstein, JR AF Greenhill, LJ Moran, JM Booth, RS Ellingsen, SP McCulloch, PM Jauncey, DL Norris, RP Reynolds, JE Tzioumis, AX Herrnstein, JR BE Schilizzi, RT Vogel, SN Paresce, F Elvis, MS TI Accretion and outflow traced by H2O masers in the circinus AGN SO GALAXIES AND THEIR CONSTITUENTS AT THE HIGHEST ANGULAR RESOLUTIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union ID ACTIVE GALACTIC NUCLEI; GALAXY; EMISSION AB The first VLBI images of H2O maser emission in the Circinus Galaxy AGN show both a warped, edge-on accretion disk and an outflow 0.1 to 1 pc from the central engine. The inferred central mass is 1.3 x 10(6) M-circle dot, while the disk mass may be on the order of 10(5) M-circle dot, based on a nearly Keplerian rotation curve. The bipolar, wide-angle outflow appears to contain "bullets" ejected from within < 0.1 pc of the central mass. The positions of filaments and bullets observed in the AGN ionization cone on kpc-scales suggest that the disk channels the flow to a radius of similar to 0.4 pc, at which the flow appears to disrupt the disk. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Onsala Space Observ, SE-43992 Onsala, Sweden. Univ Tasmania, Discipline Phys, Hobart, Tas 7001, Australia. Australia Telescope Natl Facil, Epping, NSW 2121, Australia. Renaissance Technol, E Setauket, NY 11733 USA. RP Greenhill, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Norris, Ray/A-1316-2008 OI Norris, Ray/0000-0002-4597-1906 NR 10 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-066-8 J9 IAU SYMP PY 2001 IS 205 BP 334 EP 337 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU43Z UT WOS:000175998000110 ER PT S AU Slane, P Hughes, JP Rakowski, CE Burrows, DN Nousek, JA Garmire, GP Gaensler, BM AF Slane, P Hughes, JP Rakowski, CE Burrows, DN Nousek, JA Garmire, GP Gaensler, BM BE Schilizzi, RT Vogel, SN Paresce, F Elvis, MS TI Chandra studies of supernova remnants and pulsars SO GALAXIES AND THEIR CONSTITUENTS AT THE HIGHEST ANGULAR RESOLUTIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union ID SNR RX J1713.7-3946; X-RAY-EMISSION; SHOCK ACCELERATION; CRAB-NEBULA; SHELL; DISCOVERY; EJECTA AB With sub-arcsecond angular resolution accompanied by fast time resolution and spatially resolved spectral capabilities, the Chandra X-ray Observatory provides a unique capability for the study of supernova remnants (SNRs) and pulsars. Though in its relative infancy, Chandra has already returned stunning images of SNRs which reveal the distribution of ejecta synthesized in the stellar explosions, the distinct properties of the forward and reverse shocks, and the presence of faint shells surrounding compact remnants. Pulsar observations have uncovered jet features as well as small-scaled structures in synchrotron nebulae. In this brief review we discuss results from early Chandra studies of pulsars and SNRs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010 NR 23 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-066-8 J9 IAU SYMP PY 2001 IS 205 BP 358 EP 365 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU43Z UT WOS:000175998000119 ER PT S AU Kramer, M Wex, N Kalogera, V Karastergiou, A AF Kramer, M Wex, N Kalogera, V Karastergiou, A BE Schilizzi, RT Vogel, SN Paresce, F Elvis, MS TI Asymmetric supernova explosion investigated by geodetic precession SO GALAXIES AND THEIR CONSTITUENTS AT THE HIGHEST ANGULAR RESOLUTIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union ID BINARY PULSAR B1913+16; KICKS AB We use observations and modelling of geodetic precession in the PSR B1913+16 system to obtain direct constraints on direction and magnitude of kicks imparted to the pulsar companion during the most recent supernova explosion. We find that the kick must have been directed almost perpendicular to the rotation axis of the progenitor star. C1 Univ Manchester, Jodrell Bank Observ, Manchester, Lancs, England. Max Planck Inst Radioastron, Bonn, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Kramer, M (reprint author), Univ Manchester, Jodrell Bank Observ, Manchester, Lancs, England. NR 7 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-066-8 J9 IAU SYMP PY 2001 IS 205 BP 410 EP 411 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU43Z UT WOS:000175998000135 ER PT B AU Kannappan, SJ Fabricant, DG AF Kannappan, SJ Fabricant, DG BE Funes, JG Corsini, EM TI Frequency of gas-stellar counterrotation SO GALAXY DISKS AND DISK GALAXIES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Galaxy Disks and Disk Galaxies CY JUN 12-16, 2000 CL PONTIFICAL GREGORIAN UNIV, ROME, ITALY SP Vatican Observ HO PONTIFICAL GREGORIAN UNIV ID GALAXIES AB We search for bulk counterrotation of the gas and stars in 67 galaxies of all types and a wide range of luminosities. Bulk counterrotation characterizes similar to25-30% of E/S0's with extended gas, but at most a few percent of Sa-Sbc spirals. For SO's, the frequency of counterrotation we derive agrees with previous work, but we sample significantly fainter luminosities. Thus the agreement suggests that similar formation mechanisms may operate over a wide range of physical scales. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kannappan, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-063-3 J9 ASTR SOC P PY 2001 VL 230 BP 447 EP 448 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31L UT WOS:000175667100139 ER PT B AU Kannappan, SJ Fabricant, DG AF Kannappan, SJ Fabricant, DG BE Funes, JG Corsini, EM TI Kinematic asymmetries in a broad galaxy sample SO GALAXY DISKS AND DISK GALAXIES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Galaxy Disks and Disk Galaxies CY JUN 12-16, 2000 CL PONTIFICAL GREGORIAN UNIV, ROME, ITALY SP Vatican Observ HO PONTIFICAL GREGORIAN UNIV AB We analyze asymmetries in the gas rotation curves of 113 galaxies drawn from the Nearby Field Galaxy Survey, spanning a broad range of luminosities and morphologies. If the origin of the rotation curve is chosen to minimize the asymmetry, then similar to 26% of sample galaxies show asymmetry > 5% within 1.3r(e). However, not all gas kinematic asymmetries indicate asymmetries in the underlying potential. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kannappan, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-063-3 J9 ASTR SOC P PY 2001 VL 230 BP 449 EP 450 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31L UT WOS:000175667100140 ER PT S AU Badran, HM AF Badran, HM CA VERITAS Collaboration BE Ritz, S Gehrels, N Shrader, CR TI Recent observations of 1ES2344+514 using the Whipple gamma-ray telescope SO GAMMA 2001 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Gamma-Ray Astrophysics 2001 Symposium CY APR 04-06, 2001 CL BALTIMORE, MD SP NASA, US DOE, Italian Space Agcy, TRW, Spectrum Astro, Lockheed Martin, SW Res, Orbital Sci, USRA, GLAST, Compton Gamma Ray Observ, Swift, INTEGRAL ID MULTIWAVELENGTH OBSERVATIONS; X-RAY; EMISSION; MARKARIAN-501; FLARE AB Lacertae objects are a class of AGN which are believed to be highly beamed. Very high energy gamma-rays emitted from such objects provide important information that improves our understanding of this class of objects. Only two AGNs, Mrk 421 and Mrk 50 1, are well established Tev emitters in the northern hemisphere. The Whipple collaboration previously reported a weak signal from the BL Lac object 1ES 2344+514. This object has been extensively monitored with atmospheric Cherenkov experiments from 1997 to 1999 with no other reported detection. The results of observations in 1999-2001 of 1ES 2344+514 taken with the new Whipple 490 pixel camera are presented. These observations resulted in a detection at the 3 sigma level. C1 Smithsonian Inst, Whipple Observ, Amado, AZ 85645 USA. RP Badran, HM (reprint author), Smithsonian Inst, Whipple Observ, POB 97, Amado, AZ 85645 USA. NR 22 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0027-X J9 AIP CONF PROC PY 2001 VL 587 BP 281 EP 285 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BT56P UT WOS:000173389400053 ER PT S AU Horan, D AF Horan, D CA VERITAS Collaboration BE Ritz, S Gehrels, N Shrader, CR TI Observations of the BL Lac object, 1H1426+428 at TeV gamma-ray energies SO GAMMA 2001 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Gamma-Ray Astrophysics 2001 Symposium CY APR 04-06, 2001 CL BALTIMORE, MD SP NASA, US DOE, Italian Space Agcy, TRW, Spectrum Astro, Lockheed Martin, SW Res, Orbital Sci, USRA, GLAST, Compton Gamma Ray Observ, Swift, INTEGRAL AB TeV gamma-ray observations are reported of 1H1426+428 (1H1426), an X-ray selected BL Lacertae object at a redshift of 0.129. The X-ray spectrum appears to peak near 100 keV, if this is the peak of the synchrotron emission, then this AGN is a prime candidate for TeV gamma-ray emission assuming a Compton-synchrotron model. During the 1999, 2000 and 2001 observing seasons, the source has been intensively studied with the Whipple 10m imaging atmospheric Cerenkov telescope, these observations, together with the indications from earlier observations confirm this hypothesis. The average signal was at the 4.2sigma level during the 2000 observing season, while the average signal recorded during 2001 was at the 4.9sigma level. C1 Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. RP Horan, D (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, POB 97, Amado, AZ 85645 USA. NR 10 TC 4 Z9 4 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0027-X J9 AIP CONF PROC PY 2001 VL 587 BP 324 EP 328 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BT56P UT WOS:000173389400062 ER PT S AU Silver, E Schnopper, H Jones, C Forman, W Bandler, S Murray, S Romaine, S Slane, P Grindlay, J Madden, N Beeman, J Haller, EE Smith, D Barbera, M Collura, A Christensen, F Ramsey, B Woosley, S Diehl, R Tucker, G Fabregat, J Reglero, V Gimenez, A AF Silver, E Schnopper, H Jones, C Forman, W Bandler, S Murray, S Romaine, S Slane, P Grindlay, J Madden, N Beeman, J Haller, EE Smith, D Barbera, M Collura, A Christensen, F Ramsey, B Woosley, S Diehl, R Tucker, G Fabregat, J Reglero, V Gimenez, A BE Ritz, S Gehrels, N Shrader, CR TI B-MINE, the balloon-borne microcalorimeter nuclear line explorer SO GAMMA 2001 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Gamma-Ray Astrophysics 2001 Symposium CY APR 04-06, 2001 CL BALTIMORE, MD SP NASA, US DOE, Italian Space Agcy, TRW, Spectrum Astro, Lockheed Martin, SW Res, Orbital Sci, USRA, GLAST, Compton Gamma Ray Observ, Swift, INTEGRAL ID EMISSION AB B-MINE is a concept for a balloon mission designed to probe the deepest regions of a supernova explosion by detecting Ti-44 emission at 68 keV with spatial and spectral resolutions that are sufficient to determine the extent and velocity distribution of the Ti-44 emitting region. The payload introduces the concept of focusing optics and microcalorimeter spectroscopy to nuclear line emission astrophysics. B-MINE has a thin, plastic foil telescope multilayered to maximize the reflectivity in a 20 keV band centered at 68 keV and a microcalorimeter array optimized for the same energy band. This combination provides a reduced background, an energy resolution of 50 eV and a 3sigma sensitivity in 10(6) s of 3.3 x 10(-7) ph cm(-2) s(-1) at 68 keV. During the course of a long duration balloon flight, B-MINE could carry out a detailed study of the Ti-44 emission line centroid and width in CAS A. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Silver, E (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RI Bandler, Simon/A-6258-2010 OI Bandler, Simon/0000-0002-5112-8106 NR 5 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0027-X J9 AIP CONF PROC PY 2001 VL 587 BP 860 EP 864 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BT56P UT WOS:000173389400151 ER PT S AU Weekes, TC AF Weekes, TC BE Ritz, S Gehrels, N Shrader, CR TI The next generation of ground-based gamma-ray telescopes SO GAMMA 2001 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Gamma-Ray Astrophysics 2001 Symposium CY APR 04-06, 2001 CL BALTIMORE, MD SP NASA, US DOE, Italian Space Agcy, TRW, Spectrum Astro, Lockheed Martin, SW Res, Orbital Sci, USRA, GLAST, Compton Gamma Ray Observ, Swift, INTEGRAL AB The status of ground-based gamma-ray astronomy, in terms of current and planned observatories, is reviewed. C1 Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. RP Weekes, TC (reprint author), Harvard Smithsonian Ctr Astrophys, Whipple Observ, POB 97, Amado, AZ 85645 USA. NR 10 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0027-X J9 AIP CONF PROC PY 2001 VL 587 BP 942 EP 951 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BT56P UT WOS:000173389400163 ER PT B AU Perna, R AF Perna, R BE Costa, E Frontera, F Hjorth, J TI gamma-ray burst remnants: How can we find them? SO GAMMA-RAY BURSTS IN THE AFTERGLOW ERA SE ESO ASTROPHYSICS SYMPOSIA LA English DT Proceedings Paper CT 2nd Workshop on Gamma-Ray Bursts in the Afterglow Era CY OCT 17-20, 2000 CL CNR, ROME, ITALY SP ESO, Alenia Aerosp, Laben & Nuova Telespazio HO CNR ID SUPERSHELLS; GALAXIES C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. RP Perna, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 01238 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 3-540-42771-6 J9 ESO ASTROPHY SYMP PY 2001 BP 239 EP 242 DI 10.1007/10853853_64 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BT78E UT WOS:000174050300064 ER PT J AU Haynes, CV Maxwell, TA Johnson, DL Kilani, A AF Haynes, CV Maxwell, TA Johnson, DL Kilani, A TI Research note: Acheulian sites near Bir Kiseiba in the Darb el Arba'in Desert, Egypt: New data SO GEOARCHAEOLOGY-AN INTERNATIONAL JOURNAL LA English DT Article C1 Univ Arizona, Dept Anthropol, Tucson, AZ 85721 USA. Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Univ Illinois, Dept Geog, Urbana, IL 61801 USA. Egyptian Geol Survey, Cairo, Egypt. RP Haynes, CV (reprint author), Univ Arizona, Dept Anthropol, Tucson, AZ 85721 USA. NR 2 TC 5 Z9 5 U1 0 U2 1 PU JOHN WILEY & SONS INC PI NEW YORK PA 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0883-6353 J9 GEOARCHAEOLOGY JI Geoarchaeology PD JAN PY 2001 VL 16 IS 1 BP 143 EP 150 DI 10.1002/1520-6548(200101)16:1<143::AID-GEA9>3.0.CO;2-6 PG 8 WC Archaeology; Geosciences, Multidisciplinary SC Archaeology; Geology GA 493WP UT WOS:000172246700009 ER PT B AU Falco, EE Kochanek, CS Lehar, J McLeod, BA Munoz, JA Impey, CD Keeton, C Peng, CY Rix, HW AF Falco, EE Kochanek, CS Lehar, J McLeod, BA Munoz, JA Impey, CD Keeton, C Peng, CY Rix, HW BE Brainerd, TG Kochanek, CS TI The CASTLES gravitational lensing tool SO GRAVITATIONAL LENSING: RECENT PROGRESS AND FUTURE GOALS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Gravitational Lensing - Recent Progress and Future Goals CY JUL 25-30, 1999 CL BOSTON UNIV, BOSTON, MA SP Natl Sci Fdn, NASA HO BOSTON UNIV AB We describe a series of new applications of gravitational lenses as astrophysical and cosmological tools. Such applications are becoming possible thanks to advances in the quality and quantity of observations. CASTLES (CfA-Arizona-Space-Telescope-LEns-Survey)(1) is an ongoing project that exploits the sensitivity and resolution of the Hubble Space Telescope (HST) at optical and infrared wavelengths to study the sample of over 50 known gravitational lenses. The observational goal of CASTLES is a uniform sample of multi-band images of all known galaxy-mass lens systems, to derive precise photometry and astrometry for the lens galaxies, all the known images, and any source or lens components that might have escaped detection. With these measurements we are investigating: (1) the properties of dust and of dark matter in lens galaxies out to z similar to 1; (2) the dark matter in lens galaxies and in their environments; (3) the evolution of lens galaxies; and (4) the cosmological model, for instance by refining constraints on the Hubble constant H-0. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Falco, EE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 14 TC 17 Z9 17 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-074-9 J9 ASTR SOC P PY 2001 VL 237 BP 25 EP 31 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31R UT WOS:000175678100003 ER PT B AU Munoz, JA Falco, EE Kochanek, CS Lehar, J McLeod, BA McNamara, BR Vikhlinin, AA Impey, CD Keeton, CR Peng, CY Rix, HW AF Munoz, JA Falco, EE Kochanek, CS Lehar, J McLeod, BA McNamara, BR Vikhlinin, AA Impey, CD Keeton, CR Peng, CY Rix, HW BE Brainerd, TG Kochanek, CS TI A new wide-separation gravitational lens candidate: RXJ 0921+4529 SO GRAVITATIONAL LENSING: RECENT PROGRESS AND FUTURE GOALS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Gravitational Lensing - Recent Progress and Future Goals CY JUL 25-30, 1999 CL BOSTON UNIV, BOSTON, MA SP Natl Sci Fdn, NASA HO BOSTON UNIV AB The lens candidate RXJ 0921+4529 consists of two z(S) = 1.66 quasars separated by 643 with an H band magnitude difference of Deltam = 1.39. The lens appears to be a z(1) = 0.31 X-ray cluster, including a m(H)=18.5 late-type galaxy lying between the quasar images. We detect an extended source overlapping the faint quasar but not the bright quasar. If this extended source is the host galaxy of the fainter quasar, then the system is a quasar binary rather than a gravitational lens. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Munoz, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-074-9 J9 ASTR SOC P PY 2001 VL 237 BP 49 EP 50 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31R UT WOS:000175678100010 ER PT B AU Bagla, JS AF Bagla, JS BE Brainerd, TG Kochanek, CS TI Higher order Caustics in lens models SO GRAVITATIONAL LENSING: RECENT PROGRESS AND FUTURE GOALS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Gravitational Lensing - Recent Progress and Future Goals CY JUL 25-30, 1999 CL BOSTON UNIV, BOSTON, MA SP Natl Sci Fdn, NASA HO BOSTON UNIV AB Catastrophe theory has often been used to describe generic properties of lens models, but the focus of such studies so far has been on the lower order, stable caustics such as cusps and folds. In this paper we describe the two higher order caustics and describe outline techniques that can be used to find these caustics in a given lens model. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bagla, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. NR 5 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-074-9 J9 ASTR SOC P PY 2001 VL 237 BP 77 EP 78 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31R UT WOS:000175678100020 ER PT B AU Colley, WN Schild, RE AF Colley, WN Schild, RE BE Brainerd, TG Kochanek, CS TI Hourly brightness fluctuations in Q0957+561 SO GRAVITATIONAL LENSING: RECENT PROGRESS AND FUTURE GOALS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Gravitational Lensing - Recent Progress and Future Goals CY JUL 25-30, 1999 CL BOSTON UNIV, BOSTON, MA SP Natl Sci Fdn, NASA HO BOSTON UNIV AB We have re-reduced 2000 CCD images of Q0957+561, taken over 25 nights with similar to 4 minute time resolution. Our new reduction uses HST imaging to subtract the lens galaxy accurately. We find that the quasar images vary at the few percent level during the night. To disentangle variations intrinsic to the quasar and those caused by microlensing, we have reduced data from runs separated by the now widely accepted similar to 417 day time delay. Our results suggest that the majority of the brightness fluctuations are intrinsic to the quasar, and we determine a sharpened time delay of 417.3 days. There is possibly some variation due to microlensing. If microlensing is present on these time scales, it would suggest a dark matter component in the lens galaxy which is comprised of very small (similar to 10(-5)M(circle dot)) MACHO's. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Colley, WN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-074-9 J9 ASTR SOC P PY 2001 VL 237 BP 141 EP 142 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31R UT WOS:000175678100044 ER PT B AU Kochanek, CS Falco, EE Impey, CD Lehar, J McLeod, BA Rix, HW Keeton, CR Munoz, JA Peng, CY AF Kochanek, CS Falco, EE Impey, CD Lehar, J McLeod, BA Rix, HW Keeton, CR Munoz, JA Peng, CY BE Brainerd, TG Kochanek, CS TI The evolution of gravitational lens galaxies SO GRAVITATIONAL LENSING: RECENT PROGRESS AND FUTURE GOALS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Gravitational Lensing - Recent Progress and Future Goals CY JUL 25-30, 1999 CL BOSTON UNIV, BOSTON, MA SP Natl Sci Fdn, NASA HO BOSTON UNIV ID FUNDAMENTAL PLANE; COSMOLOGICAL CONSTANT; ELLIPTICAL GALAXIES; MERGER MODEL; SPECTROSCOPY; CLUSTERS; PHOTOMETRY AB Most gravitational lens galaxies are early-type galaxies in relatively low density environments. We show that they lie on the same fundamental plane as early-type galaxies in both local and distant rich clusters. Their surface brightness evolution requires a typical star formation epoch of z(f) similar or equal to 2-3, almost indistinguishable from that of rich cluster galaxies at comparable redshifts. The restricted galaxy type range of the lenses means that photometric redshifts work well even with only 1-3 filter photometry. We make preliminary measurements of the mass and luminosity functions of the lens galaxies, and find they are consistent with the standard model used for deriving cosmological limits using lens statistics. As expected for a mass-weighted sample, they are more massive and more luminous than the overall early-type galaxy population. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kochanek, CS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 28 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-074-9 J9 ASTR SOC P PY 2001 VL 237 BP 159 EP 168 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31R UT WOS:000175678100053 ER PT B AU McLeod, BA Falco, EE Kochanek, CS Lehar, J Munoz, JA Impey, CD Keeton, C Peng, CY Rix, HW AF McLeod, BA Falco, EE Kochanek, CS Lehar, J Munoz, JA Impey, CD Keeton, C Peng, CY Rix, HW BE Brainerd, TG Kochanek, CS TI The interstellar medium of lens galaxies SO GRAVITATIONAL LENSING: RECENT PROGRESS AND FUTURE GOALS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Gravitational Lensing - Recent Progress and Future Goals CY JUL 25-30, 1999 CL BOSTON UNIV, BOSTON, MA SP Natl Sci Fdn, NASA HO BOSTON UNIV ID GRAVITATIONAL LENSES; EXTINCTION; ABSORPTION; SUPERNOVAE AB We use observations from the CASTLES survey of gravitational. lenses to study extinction in 23 lens galaxies with 0 < z(l) < 1. The median differential extinction between lensed images is DeltaE(B - V) = 0.05 mag, and the directly measured extinctions agree with the amount needed to explain the differences between the statistics of radio and (optical) quasar lens surveys. We also measure the first extinction laws outside the local universe, including an R-V = 7.2 curve for a molecular cloud at z(l) = 0.68 and an R-V = 1.5 curve for the dust in a redshift z(l) = 0.96 elliptical galaxy. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McLeod, BA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 13 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-074-9 J9 ASTR SOC P PY 2001 VL 237 BP 177 EP 180 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31R UT WOS:000175678100055 ER PT J AU Wilson, DS Nagy, KA Tracy, CR Morafka, DJ Yates, RA AF Wilson, DS Nagy, KA Tracy, CR Morafka, DJ Yates, RA TI Water balance in neonate and juvenile desert tortoises, Gopherus agassizii SO HERPETOLOGICAL MONOGRAPHS LA English DT Article DE Gopherus agassizii; burrow refuge; dehydration; doubly labeled water; evaporation; hibernation; humidity effect; neonate; juvenile ID HUMIDITY ACCLIMATION; ANOLIS-CAROLINENSIS; 2 POPULATIONS AB We examined evaporative water loss of neonate (<1 yr old) tortoises in laboratory experiments designed to evaluate the dependence of evaporation oil humidity, and of juvenile (1-4 yr old) tortoises in field experiments designed to reveal the influence of burrow microclimate oil water gain and loss. in controlled laboratory conditions, rates of body mass loss which reflect net evaporative water losses, were independent of the difference in vapor density between the animal and its environment. Changes in skin permeability and respiratory parameters may, account for this. Sleeping tortoises lost body mass half as fast as did active tortoises and hibernating individuals lost body mass 1/20(th) as quickly as active animals. juveniles confined to short (20 cm) or long (70 cm) burrows in the field lost body mass faster in the drier and warmer short burrows. Doubly labeled water was used in tortoises residing in different burrow types to measure total (unidirectional) rates of evaporation, vapor influx and metabolic water production, to partition net water loss (as reflected in body mass loss) into its parts. Total evaporation rate was independent of burrow conditions, but tortoises in the longer, more humid burrows had higher rates of water vapor input and total water input than did those in shorter burrows. Thus, tortoises in long burrows lost body mass more slowly in response to a higher humidity, in contrast to neonates under laboratory conditions, Rates or body mass loss due to evaporation from neonates were relatively high in the laboratory (0.4 to 0.8 % of body mass per day) and the field (0.7 to 1.1 %/d compared to those, of adults in the laboratory (0.17 %/d) or the field (0.1 %/d). Thus, young tortoises apparently are obliged to rely oil behavioral means (drinking pooled rain, withdrawing into their shell, seeking long, deep burrows) to avoid lethal dehydration in relatively hot, dry seasons. C1 Univ Nevada, Biol Resources Res Ctr, Reno, NV 89557 USA. Univ Calif Los Angeles, Dept Biol, Los Angeles, CA 90024 USA. Calif State Univ Dominguez Hills, Dept Biol, Carson, CA 90747 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Wilson, DS (reprint author), Calif State Univ Los Angeles, Dept Biol Sci, Chico, CA 95929 USA. NR 37 TC 12 Z9 12 U1 3 U2 5 PU HERPETOLOGISTS LEAGUE PI EMPORIA PA EMPORIA STATE UNIV, DIVISION BIOLOGICAL SCIENCES, 1200 COMMERCIAL ST, EMPORIA, KS 66801-5087 USA SN 0733-1347 EI 1938-5137 J9 HERPETOL MONOGR JI Herpetol. Monogr. PY 2001 VL 15 BP 158 EP 170 DI 10.2307/1467042 PG 13 WC Zoology SC Zoology GA 470QR UT WOS:000170883100006 ER PT S AU Weekes, TC AF Weekes, TC BE Aharonian, FA Volk, HJ TI Status of VHE astronomy c.2000 SO HIGH ENERGY GAMMA-RAY ASTRONOMY SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT International Symposium on High Energy Gamma-Ray Astronomy CY JUN 26-30, 2000 CL HEIDELBERG UNIV, HEIDELBERG, GERMANY SP Max Planck Inst Kernphys, DFG, Int Union Pure & Appl Phys HO HEIDELBERG UNIV ID GAMMA-RAY ASTRONOMY; CHERENKOV TELESCOPE; TEV; HEGRA C1 Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. RP Weekes, TC (reprint author), Harvard Smithsonian Ctr Astrophys, Whipple Observ, POB 97, Amado, AZ 85645 USA. NR 42 TC 19 Z9 19 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 1-56396-990-4 J9 AIP CONF PROC PY 2001 VL 558 BP 15 EP 26 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS12B UT WOS:000168728000002 ER PT S AU Noble, MS Zlateva, S AF Noble, MS Zlateva, S BE Hertzberger, B Hoekstra, A Williams, R TI Scientific computation with JavaSpaces SO HIGH-PERFORMANCE COMPUTING AND NETWORKING SE LECTURE NOTES IN COMPUTER SCIENCE LA English DT Article; Proceedings Paper CT 9th International Conference on High-Performance Computing and Networking CY JUN 25-27, 2001 CL AMSTERDAM, NETHERLANDS AB JavaSpaces provides a simple yet expressive mechanism for distributed computing with commodity technology. We discuss the suitability of JavaSpaces for implementing different classes of concurrent computations based on low-level metrics (null messaging and array I/O), and present performance results for several parametric algorithms. We found that although inefficient for communication intensive problems, JavaSpaces yields good speedups for parametric experiments, relative to both sequential Java and C. We also outline a dynamic native compilation technique, which for short, compute-intensive codes further boosts performance without compromising Java portability or extensive algorithm recoding. Discussion and empirical results are presented in the context of our public benchmark suite. C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Boston Univ, Boston, MA 02215 USA. RP Noble, MS (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 13 TC 5 Z9 5 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-42293-5 J9 LECT NOTES COMPUT SC PY 2001 VL 2110 BP 657 EP 666 PG 10 WC Computer Science, Information Systems; Computer Science, Theory & Methods SC Computer Science GA BV76G UT WOS:000179960900075 ER PT J AU Owsley, DW AF Owsley, DW TI Why the forensic anthropologist needs the archaeologist SO HISTORICAL ARCHAEOLOGY LA English DT Article AB Many scientific experts and specialists can be invited to join a forensic anthropology team and are used effectively in cases involving missing persons and buried homicide victims, as well as in locating historic burials. Nevertheless, the most significant addition to a forensic anthropology team is the archaeologist. The archaeologist is often instrumental in solving the puzzle of the burial's location, which can lead to resolving the riddle of the deceased person's identification and cause of death. This specialist's training and experience with various soils and the environmental context surrounding buried or scattered remains makes his services invaluable to the leader of a well-rounded and successful forensic team. This article highlights the importance of archaeological expertise and its use in the forensic investigation. C1 Smithsonian Inst, Museum Natl Hist Nat, Washington, DC 20560 USA. RP Owsley, DW (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Washington, DC 20560 USA. NR 0 TC 6 Z9 6 U1 0 U2 4 PU SOC HISTORICAL ARCHAEOLOGY PI TUCSON PA PO BOX 30446, TUCSON, AZ 85751-0446 USA SN 0440-9213 J9 HIST ARCHAEOL JI Hist. Archaeol. PY 2001 VL 35 IS 1 BP 35 EP 38 PG 4 WC Archaeology SC Archaeology GA 414KF UT WOS:000167665000004 ER PT S AU Hunt, DR AF Hunt, DR BE Williams, E TI The value of human remains for research and education SO HUMAN REMAINS: CONSERVATION, RETRIEVAL, AND ANALYSIS, PROCEEDINGS SE BRITISH ARCHAEOLOGICAL REPORTS INTERNATIONAL SERIES (SUPPLEMENTARY) LA English DT Proceedings Paper CT Conference on Human Remains - Conservation, Retrieval and Analysis CY NOV 07-11, 1999 CL WILLIAMSBURG, VA ID TYROLEAN ICE MAN; HISTORY AB Preserved human remains provide valuable and in some instances unique opportunities to study individuals from prehistoric and historic periods. Skeletal remains provide a rich and valuable source of information about past peoples. Mummified remains provide the biological anthropologist with even deeper detail through investigations of soft tissue anatomy, parasitology, infectious or toxic afflictions, and interpretation of congenital or malignant pathological conditions. With advancements in sophisticated analytical technologies such as mtDNA, nuclear DNA, various isotopic and elemental analyses, scanning electron microscopy and computerized tomography, new research capabilities appear limitless. Therefore, the preservation of both skeletal and mummified collections of human remains, combined with better efforts to disseminate the information retrieved, has become imperative. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 55 TC 1 Z9 1 U1 0 U2 1 PU BRITISH ARCHAEOL REPORTS ARCHAEOPRESS PI OXFORD PA P O BOX 920, OXFORD OX27YH, ENGLAND SN 0143-3059 BN 1-84171-228-0 J9 BRIT ARCHAEOL REP IN PY 2001 VL S934 BP 129 EP 134 PG 6 WC Anthropology; Archaeology SC Anthropology; Archaeology GA BV35X UT WOS:000178669000019 ER PT S AU Bruwelheide, KS Beck, J Pelot, S AF Bruwelheide, KS Beck, J Pelot, S BE Williams, E TI Standardized protocol for radiographic and photographic documentation of human skeletons SO HUMAN REMAINS: CONSERVATION, RETRIEVAL, AND ANALYSIS, PROCEEDINGS SE BRITISH ARCHAEOLOGICAL REPORTS INTERNATIONAL SERIES (SUPPLEMENTARY) LA English DT Proceedings Paper CT Conference on Human Remains - Conservation, Retrieval and Analysis CY NOV 07-11, 1999 CL WILLIAMSBURG, VA ID COMPUTED-TOMOGRAPHY; SKULLS; LINES AB The Repatriation Osteology Laboratory of the Smithsonian Institution follows a rigorous protocol of data collection on human skeletal remains involving standardized radiographic and photographic documentation. Over 15,000 radiographs and 63, 000 photographs have been compiled, creating one of the world's largest visual data sets for a museum skeletal collection. The benefits of this record are both immediate and long term. The ability to review radiographs alongside the skeletal remains allows physical anthropologists to perform more detailed examination of pathological conditions, provides visual markers for nutritional deficiencies and disease stress, facilitates in age assessment of sub-adults, and aids in the evaluation of antemortem versus postmortem modifications of bone. Long-term benefits of radiographic and photographic records include the presence of a large standardized visual data set available for continued reference by museum personnel and future researchers as techniques evolve and collections are lost to repatriation. The presence of a visual record has also proven useful to the collections management aspect of museum curation. Photographs and radiographs of museum specimens have provided a check against written accession records as to the presence or absence of remains and their condition. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Repatriat Off, Washington, DC 20560 USA. NR 29 TC 1 Z9 2 U1 0 U2 3 PU BRITISH ARCHAEOL REPORTS ARCHAEOPRESS PI OXFORD PA P O BOX 920, OXFORD OX27YH, ENGLAND SN 0143-3059 BN 1-84171-228-0 J9 BRIT ARCHAEOL REP IN PY 2001 VL S934 BP 153 EP 165 PG 13 WC Anthropology; Archaeology SC Anthropology; Archaeology GA BV35X UT WOS:000178669000022 ER PT S AU Ousley, S McKeown, A AF Ousley, S McKeown, A BE Williams, E TI Three dimensional digitizing of human skulls as an archival procedure SO HUMAN REMAINS: CONSERVATION, RETRIEVAL, AND ANALYSIS, PROCEEDINGS SE BRITISH ARCHAEOLOGICAL REPORTS INTERNATIONAL SERIES (SUPPLEMENTARY) LA English DT Proceedings Paper CT Conference on Human Remains - Conservation, Retrieval and Analysis CY NOV 07-11, 1999 CL WILLIAMSBURG, VA ID DISTANCE MATRIX ANALYSIS; CRANIOMETRIC VARIATION; HUMAN-POPULATIONS; CRANIA AB Recent hardware and software developments have made the collection of three-dimensional (3D) data more convenient and affordable. Collecting 3D data using a digitizer has several advantages over collecting conventional craniometric data using standard instruments that make it ideal for archival, research, and repatriation purposes: 1. It can be not much more expensive ($3000) than purchasing the equivalent conventional craniometric instruments ($2200 and up). 2. It records cranial morphology far better than one-dimensional measurements. 3. Data can be collected much faster than using conventional instruments. 4. It can be converted into conventional (Howells/Martin) cranial measurements for use with previously collected data using 3 Skull software. 5. It records data with fewer errors because all relevant data can be electronically transmitted and calculated. 6. A missing bilateral landmark can be estimated, if one is present, and related measurements can be calculated. Additionally, statistical advances have provided more dsophisticated methods of analyzing 3D coordinate data. C1 Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 52 TC 6 Z9 7 U1 0 U2 4 PU BRITISH ARCHAEOL REPORTS ARCHAEOPRESS PI OXFORD PA P O BOX 920, OXFORD OX27YH, ENGLAND SN 0143-3059 BN 1-84171-228-0 J9 BRIT ARCHAEOL REP IN PY 2001 VL S934 BP 173 EP 184 PG 12 WC Anthropology; Archaeology SC Anthropology; Archaeology GA BV35X UT WOS:000178669000024 ER PT J AU Reid, JW AF Reid, JW TI A human challenge: discovering and understanding continental copepod habitats SO HYDROBIOLOGIA LA English DT Review DE Cyclopoida; Harpacticoida; habitats; leaf litter; phytotelmata; artificial habitats; review ID STEGOMYIA POLYNESIENSIS MARKS; CYCLOPOID COPEPODS; HARPACTICOID COPEPODS; JAMAICAN BROMELIADS; BIOLOGICAL-CONTROL; SPECIES COPEPODA; 1951 DIPTERA; PUERTO-RICO; CRAB HOLES; CRUSTACEA AB Copepods have invaded an astonishing variety of aquatic and humid continental environments and microhabitats. The historical process of discovery and investigation of copepods in ephemeral, acid and thermal waters, subterranean waters and sediments, phytotelmata, humid soils, leaf litter, human-modified and artificial habitats, and other situations extends over about 130 years. The methods developed to collect in and study these habitats range from simple nets to elaborate pumping systems and diving techniques. Investigations of non-lacustrine continental environments have contributed greatly to the understanding of aspects of copepod biology such as reproduction, diapause and population dynamics. Questions regarding faunistics and biological diversity, biogeography, evolution, transport and introductions of alien species have also been informed by such studies. This article briefly reviews these topics, and provides detailed lists of records from some of the less well-known kinds of habitats. C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Systemat Biol Invertebrate Zool, Washington, DC 20560 USA. RP Reid, JW (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Systemat Biol Invertebrate Zool, Washington, DC 20560 USA. EM reid.janet@nmnh.si.edu NR 279 TC 41 Z9 44 U1 4 U2 18 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PY 2001 VL 453 IS 1-3 BP 201 EP 226 DI 10.1023/A:1013148808110 PG 26 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 499ZD UT WOS:000172600200018 ER PT J AU Bruno, MC Loftus, WF Reid, JW Perry, SA AF Bruno, MC Loftus, WF Reid, JW Perry, SA TI Diapause in copepods (Crustacea) from ephemeral habitats with different hydroperiods in Everglades National Park (Florida, USA) SO HYDROBIOLOGIA LA English DT Article DE copepods; diapause; ephemeral habitats; pre-fertilized females; Everglades; wetlands ID LIFE-CYCLE; CYCLOPOID COPEPODS; FRESH-WATERS; DYNAMICS; MESOCYCLOPS; POPULATION; EMERGENCE; PATTERNS; POND; ZOOPLANKTON AB Water management practices in the Everglades have severely stressed the natural system, particularly by reducing the hydroperiods of much of the region. During the dry season of 1999, we investigated the influence of hydroperiod on the species composition and dormancy patterns of freshwater copepod communities in seasonal wetlands of Everglades National Park, Florida, U.S.A. The habitats were characterized by an annual dry season, from December through June. We sampled at two locations: the Long Pine Key area of the Rocky Glades region (short hydroperiod, ca. 4-5 months), and western Taylor Slough (intermediate hydroperiod, ca. 8-10 months). Both areas have experienced a reduction in natural hydroperiods and an increase in the frequency of dry-down. We collected weekly plankton samples from Rocky Glades solution holes to assess the potential species pool of copepods. To document the taxa capable of surviving dry-down by resting, we performed three immersion trials in which we rehydrated, in laboratory aquaria, sediment patches from solution holes and surface soils from all stations. Only a subset of the planktonic species collected emerged from the dried sediments. The cyclopoids Microcyclops rubellus and Paracyclops poppei were dominant. This is the first record of diapause for P. poppei. Species distributions from the different hydroperiod soil patches indicated that more diapausing species occurred at the sites that dried for shorter periods. Emerging individuals of M. rubellus and P. poppei were mainly ovigerous females, demonstrating a resting strategy seldom before recorded. The cyclopoid Diacyclops nearcticus had not been previously reported to diapause, but they emerged from the dried sediments in our trials. Our collections included six new records for Florida: Diacyclops nearcticus, Megacyclops latipes, Orthocyclops modestus, Elaphoidella marjoryae, Bryocamptus sp. and Bryocamptus cf. newyorkensis. Paracyclops poppei, Macrocyclops fuscus and Arctodiaptomus floridanus are new records for Everglades National Park. Clearly, diapause is an important strategy for the persistence of copepods in short-hydroperiod wetlands. The duration of the dry period appears to be inversely related to the number of species that emerge from diapause. C1 S Florida Nat Resources Ctr, Homestead, FL 33034 USA. US Geol Survey, Biol Resources Div, Homestead, FL 33034 USA. Smithsonian Inst, Natl Museum Amer Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Bruno, MC (reprint author), S Florida Nat Resources Ctr, Everglades Natl Pk, Homestead, FL 33034 USA. RI Bruno, Maria Cristina/D-8792-2011; Bruno, Maria Cristina/B-8117-2015 OI Bruno, Maria Cristina/0000-0001-7860-841X; Bruno, Maria Cristina/0000-0001-7860-841X NR 65 TC 22 Z9 23 U1 1 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 EI 1573-5117 J9 HYDROBIOLOGIA JI Hydrobiologia PY 2001 VL 453 IS 1-3 BP 295 EP 308 DI 10.1023/A:1013161210836 PG 14 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 499ZD UT WOS:000172600200024 ER PT J AU Tanaka, H Roubik, DW Kato, M Liew, F Gunsalam, G AF Tanaka, H Roubik, DW Kato, M Liew, F Gunsalam, G TI Phylogenetic position of Apis nuluensis of northern Borneo and phylogeography of A-cerana as inferred from mitochondrial DNA sequences SO INSECTES SOCIAUX LA English DT Article DE honey bees; Apis nuluensis; phylogeny; speciation; mtDNA ID HONEY-BEES HYMENOPTERA; MTDNA VARIATION; DRONE FLIGHT; VECHTI MAA; APIDAE; MELLIFERA; EVOLUTION; GENE; BIOGEOGRAPHY; INSIGHTS AB The montane honeybee, Apis nuluensis, is adapted to the Mt. Kinabalu highlands of Borneo. We analyzed the phylogenetic position of this bee using three mitochondrial genes, 16S ribosomal RNA(16S)and cytochrome oxidases subunit 1 and 2 (CO1 and CO2). The earlier suggestion that A. nuluensis is closely related to A. cerana was supported. We showed that this honeybee may derive from an isolated population of honeybees that colonized Borneo during Plio-Pleistocene glaciations. Based on the divergence rate for silent sites of mtDNA (2.3% per Ma), the population division between A. nuluensis and A. cerana in Borneo occurred between 0.5 Ma (from 16S) and 2.4 Ma (from CO1). Large inconsistencies in the application of CO2 in the phylogenetic analysis of Apis were found. Geographic radiation of the eastern hive bee, Apis cerana, occurred in unison with divergence, which led to the speciation of Apis nuluensis. C1 Kyoto Univ, Ctr Ecol Res, Shiga 5202113, Japan. Smithsonian Trop Res Inst, Balboa, Panama. Kyoto Univ, Grad Sch Human & Environm Studies, Kyoto, Japan. Sabah Parks, Kota Kinabalu 88806, Sabah, Malaysia. RP Tanaka, H (reprint author), Kyoto Univ, Ctr Ecol Res, Shiga 5202113, Japan. NR 54 TC 38 Z9 42 U1 3 U2 12 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PY 2001 VL 48 IS 1 BP 44 EP 51 DI 10.1007/PL00001744 PG 8 WC Entomology SC Entomology GA 418LL UT WOS:000167893600008 ER PT J AU Arnoldi, MJ AF Arnoldi, MJ TI Legends, sorcerers, and enchanted lizards: Door locks of the Bamana of Mali SO INTERNATIONAL JOURNAL OF AFRICAN HISTORICAL STUDIES LA English DT Book Review C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Arnoldi, MJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AFRICAN STUDIES CENTER PI BOSTON PA BOSTON UNIVERSITY 270 BAY STATE ROAD, BOSTON, MA 02215 USA SN 0361-7882 J9 INT J AFR HIST STUD JI Int. J. Afr. Hist. Stud. PY 2001 VL 34 IS 3 BP 724 EP 725 DI 10.2307/3097602 PG 2 WC History SC History GA 598WQ UT WOS:000178299800053 ER PT J AU Bush, T AF Bush, T TI Tritobia Benjamin: Following on Porter's footsteps (Scholar in African American art) SO INTERNATIONAL REVIEW OF AFRICAN AMERICAN ART LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. RP Bush, T (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU MUSEUM AFR AMER ART PI LOS ANGELES PA 4005 CRENSHAW BLVD, LOS ANGELES, CA 90008-2534 USA SN 1045-0920 J9 INT REV AFR AM ART JI Int. Rev. Afr. Am. Art PY 2001 VL 18 IS 1 BP 16 EP 17 PG 2 WC Art SC Art GA 500PN UT WOS:000172636100004 ER PT J AU Pechenik, JA Rice, ME AF Pechenik, JA Rice, ME TI Influence of delayed metamorphosis on postsettlement survival and growth in the sipunculan Apionsoma misakianum SO INVERTEBRATE BIOLOGY LA English DT Article DE KCl; larvae; metamorphosis; potassium; sipunculans ID HYDROIDS-ELEGANS HASWELL; BUGULA-NERITINA BRYOZOA; GASTROPOD CREPIDULA-FORNICATA; LARVAL SWIMMING DURATION; 3 CHEMICAL CUES; CAPITELLA-SP-I; STRONGYLOCENTROTUS-DROEBACHIENSIS; BALANUS-AMPHITRITE; PHESTILLA-SIBOGAE; POSTLARVAL GROWTH AB Certain stresses experienced by marine larvae from many groups can dramatically reduce aspects of juvenile performance. This study reports the effects of delayed metamorphosis and nutritional stress on survival and growth of the deposit-feeding sipunculan Apionsoma (= Golfingia) misakianum. Approximately 600 larvae collected from the Florida Current plankton were distributed among 3 treatment groups. Ninety larvae (controls) were offered sediment and adult-conditioned seawater 4 d after collection, to induce metamorphosis; larvae of this species could not be induced to metamorphose by increasing the K+ concentration of seawater. The remaining 500 larvae were kept swimming for either 2 or 4 weeks, with or without phytoplankton (clone T-ISO). At the end of the periods of prolonged larval swimming, subsampled larvae (360) were induced to metamorphose as in the controls. Surviving individuals were retrieved 6 weeks after the addition of excess sediment in all treatments, and weighed to document growth. Neither delayed metamorphosis nor starvation influenced juvenile survival. However, starving larvae for 2 weeks significantly reduced mean juvenile growth rates relative to the mean growth rate of control individuals (p<0.0001), while prolonging larval life by 4 weeks significantly reduced mean juvenile growth rates (p<0.05) whether or not larvae were fed. Reduced juvenile growth rates may have been caused by nutritional stress experienced by larvae in both the starved and fed treatments. The rapid response of freshly collected larvae to sediment indicates that competent larvae of this species routinely delay metamorphosis in the field. The extent to which they also experience food limitation is not yet clear. If competent larvae are food limited while delaying metamorphosis in the field, our results suggest that juveniles will grow more slowly and may thus exhibit reduced fitness. C1 Tufts Univ, Dept Biol, Medford, MA 02155 USA. Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Pechenik, JA (reprint author), Tufts Univ, Dept Biol, Medford, MA 02155 USA. EM Jan.Pechenik@tufts.edu NR 63 TC 19 Z9 20 U1 1 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1077-8306 EI 1744-7410 J9 INVERTEBR BIOL JI Invertebr. Biol. PY 2001 VL 120 IS 1 BP 50 EP 57 PG 8 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 424ZV UT WOS:000168264600005 ER PT J AU Schwartz, ML Dimock, RV AF Schwartz, ML Dimock, RV TI Ultrastructural evidence for nutritional exchange between brooding unionid mussels and their glochidia larvae SO INVERTEBRATE BIOLOGY LA English DT Article DE bivalvia; Utterbackia; Pyganodon; matrotrophy; gills ID FRESH-WATER MUSSEL; SCANNING ELECTRON-MICROSCOPY; LIGUMIA-SUBROSTRATA; PYGANODON-CATARACTA; UNIONACEA BIVALVIA; ANODONTA-ANATINA; CALCIUM; GILLS; HISTOCHEMISTRY; METAMORPHOSIS AB The life history of unionid bivalve molluscs includes retention of developing embryos within the gills of parental mussels. This brooding behavior may facilitate nutrient transfer to the glochidia larvae, i.e., matrotrophy. To address this possibility, morphological relationships between brood chambers and developing larvae of Pyganodon cataracta and Utterbackia imbecillis were examined with TEM, and larval shells were observed with SEM, for features that could be associated with the uptake of dissolved materials. Early in brooding, glochidia are enclosed in a vitelline membrane that physically contacts numerous cilia and microvilli of the epithelia] cells lining the brood chamber (marsupium). The vitelline membrane subsequently disappears. Lamellar tissues of parental mussels initially have large deposits of glycogen that diminish during the course of brooding. Septa separating brood chambers from adjacent secondary water tubes have numerous mitochondria and microvilli, suggesting the potential for active transport of materials into or out of the marsupia. Since punctae (pores) in the larval shells become filled with an organic matrix early in brooding, they are unlikely to be involved in nutrient exchange. Ultrastructure of the brood chamber and physical contact between the parental mussel and larvae are consistent with a nutritive role for retention of glochidia in the marsupia. C1 Wake Forest Univ, Dept Biol, Winston Salem, NC 27109 USA. RP Schwartz, ML (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. NR 46 TC 32 Z9 34 U1 2 U2 14 PU AMER MICROSCOPICAL SOC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 1077-8306 J9 INVERTEBR BIOL JI Invertebr. Biol. PY 2001 VL 120 IS 3 BP 227 EP 236 DI 10.1111/j.1744-7410.2001.tb00033.x PG 10 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 466JC UT WOS:000170641600004 ER PT S AU Kensley, B AF Kensley, B BE Kensley, B Brusca, RC TI Biogeography of the marine Isopoda of the Indian Ocean, with a check-list of species and records SO ISOPOD SYSTEMATICS AND EVOLUTION SE CRUSTACEAN ISSUES LA English DT Proceedings Paper CT 2nd International Isopod Conference CY JUL 16-17, 1998 CL AMSTERDAM, NETHERLANDS ID CIROLANID ISOPOD; SOUTHERN AUSTRALIA; CRUSTACEA; GENUS; SPHAEROMATIDAE; PERACARIDA; CERCEIS; SEA AB The marine isopod fauna of the Indian Ocean is reviewed in terms of its species diversity and biogeography. For the purposes of the review, the northeastern boundary of the Indian Ocean is defined at Cape Talpot in northern Western Australia and at Rottnest Island/Perth in southern Western Australia. The history of isopod systematics in the Indian Ocean is reviewed by region, and the great lack of knowledge for Madagascar, parts of Western Australia, the east coast of Africa, and the continental shelf/slope overall, is noted. Previous research on the biogeographical provinces or regions of the Indian Ocean is briefly reviewed. For some groups of organisms, an impression of overall homogeneity for the tropical-subtropical area may prevail. However, close examination dispels the idea of homogeneity, and a number of sub-provinces or regions can be characterized. For a biogeographic review of the Indian Ocean marine isopods, a species list was compiled, which includes as many records for each species as could be found. This list contains approximately 1000 species in 303 genera. About 84% of the species are endemic to the Indian Ocean overall, but only 18% of the genera, a pattern consistent with the geological history especially of the Tethys Sea and the evolution of the Indian Ocean. This pattern is also consistent for a benthic-dwelling group which lacks a pelagic stage and whose juveniles emerge from the brood-pouch as small versions of the adults. More than half the species are known from only a single record. Seven sub-provinces or regions are characterized in terms of their isopod fauna: 1. Sub-Antarctic Region, 79% of 135 species are endemic; 2. South African Region, 68% of 226 species are endemic; 3. Western Australia Region, 58% of 115 species are endemic; 4. East African Region, 46% of 144 species are endemic; 5. Red Sea Region, 63% of 105 species are endemic; 6. Indian Region, 62% of 268 species are endemic; and 7. Madagascar Region, 63% of 168 species are endemic. These levels of endemism are higher than those seen for most organisms for which data exist. C1 Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20560 USA. RP Kensley, B (reprint author), Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20560 USA. NR 428 TC 43 Z9 47 U1 0 U2 0 PU A A BALKEMA PUBLISHERS PI LEIDEN PA SCHIPHOLWEG 107C, PO BOX 447, 2316 XC LEIDEN, NETHERLANDS SN 0168-6356 BN 90-5809-327-1 J9 CRUSTACEAN ISS JI Crustacean Iss. PY 2001 VL 13 BP 205 EP 264 PG 60 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BS24M UT WOS:000169154800006 ER PT J AU Terwilliger, VJ Kitajima, K Le Roux-Swarthout, DJ Mulkey, S Wright, SJ AF Terwilliger, VJ Kitajima, K Le Roux-Swarthout, DJ Mulkey, S Wright, SJ TI Influences of heterotrophic and autotrophic resource use on carbon and hydrogen isotopic compositions of tropical tree leaves SO ISOTOPES IN ENVIRONMENTAL AND HEALTH STUDIES LA English DT Article DE carbon isotopes; hydrogen isotopes; tropical trees; leaf development; carbon use ID AMAZONIAN RAIN-FOREST; PHASEOLUS-VULGARIS L; LEAF WATER; DELTA-C-13 VALUES; DRY FOREST; NATURAL-ABUNDANCE; WALNUT SEEDLINGS; FRENCH-GUIANA; PLANTS; CELLULOSE AB The delta C-13 and deltaD values of newly emerging to senescing tree leaves produced during a rainy season were obtained in dry seasonal and moist forest in Panama. Newly emerging leaves had less negative delta C-13 values than older leaves yet instantaneous p(i)/p(a) was never lowest in the youngest leaves. Furthermore, isotopic enrichment during early growth may have a detectable influence on the delta C-13 values of mature leaves. The deltaD values ofcellulose nitrate were only related to deltaD values of leaf water if leaf age was also considered so that, for a given deltaD of leaf water, deltaD values were highest in the youngest leaves (R-2 = 98%). There was no correlation between leaf age and deltaD values of leaf water. Investment of translocated organic carbon is a factor likely to be associated with both C-13 and deuterium enrichment effects in new leaves. A coarse, mass balance approach can estimate the proportional heterotrophic investment in leaf growth and improve estimates of integrated p(i)/p(a) by approximating delta C-13 for the most autotrophic phase of leaf growth. delta C-13 values of the predominantly sucrose mobile organic fraction in new leaves were less negative than in older leaves, thereby suggesting that the enrichment did not occur at the original site of production of the substrate for new leaf growth. Although the delta values of early leaf growth must be influenced by inputs of translocated organic carbon, enrichment effects, per se, are apparently caused by other mechanisms such as, for carbon, de novo sucrose synthesis and anaplerotic replenishment. Better recognition of metabolic causes of isotopic enrichment in leaves promises to increase the power and accuracy of inferences about carbon and water use of tropical trees from delta analyses. C1 Univ Kansas, Dept Geog, Lawrence, KS 66045 USA. Univ Florida, Dept Bot, Gainesville, FL 32611 USA. Univ Arkansas, Dept Biol Sci, Fayetteville, AR 72701 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Terwilliger, VJ (reprint author), Univ Kansas, Dept Geog, Lawrence, KS 66045 USA. RI Kitajima, Kaoru/E-8877-2012; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 77 TC 9 Z9 9 U1 0 U2 5 PU GORDON BREACH PUBLISHING, TAYLOR & FRANCIS GROUP PI PHILADELPHIA PA 325 CHESTNUT ST, 8TH FL, PHILADELPHIA, PA 19106 USA SN 1025-6016 J9 ISOT ENVIRON HEALT S JI Isot. Environ. Health Stud. PY 2001 VL 37 IS 2 BP 133 EP 160 DI 10.1080/10256010108033289 PG 28 WC Chemistry, Inorganic & Nuclear; Environmental Sciences SC Chemistry; Environmental Sciences & Ecology GA 490VX UT WOS:000172075400005 PM 11761402 ER PT J AU Rice, RA AF Rice, RA TI Noble goals and challenging terrain: Organic and fair trade coffee movements in the global marketplace SO JOURNAL OF AGRICULTURAL & ENVIRONMENTAL ETHICS LA English DT Article DE alternative trading organizations; certified organic; coffee; fair trade AB Social relations associated with conventional agricultural exports find their origins in long term associations based on business, family, and class alliances. Working outside these boundaries presents a host of challenges, especially where small producers with little economic or political power are concerned. Yet, in many developing countries, alternative trade organizations (ATOs) based on philosophies of social justice and/or environmental well-being are carving out spaces alongside traditional agricultural export sectors by establishing new channels of trade and marketing. Coffee provides a case in point, with the fair trade and certified organic movements making inroads into the market place. In their own ways, these movements represent a type of economic and social restructuring from below, drawing upon and developing linkages beyond the traditional boundaries of how coffee is produced and traded. An examination of the philosophies of the fair trade and organic coffee movements reveal that the philosophical underpinnings of both certified organic and fair-trade coffee run counter to the historical concerns of coffee production and trade. Associations of small producers involved in these coffees face stiff challenges - both internal and external to their groups. More work, especially in situ fieldwork aimed at uncovering the challenges, benefits, tensions, and successes, is needed to understand better the ways these networks operate in the dynamic agro-food complex. C1 Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Rice, RA (reprint author), Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. NR 63 TC 60 Z9 63 U1 0 U2 21 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 1187-7863 J9 J AGR ENVIRON ETHIC JI J. Agric. Environ. Ethics PY 2001 VL 14 IS 1 BP 39 EP 66 DI 10.1023/A:1011367008474 PG 28 WC Agriculture, Multidisciplinary; Ethics; Environmental Sciences; History & Philosophy Of Science SC Agriculture; Social Sciences - Other Topics; Environmental Sciences & Ecology; History & Philosophy of Science GA 419AD UT WOS:000167926400003 ER PT J AU Eberhard, WG AF Eberhard, WG TI Under the influence: Webs and building behavior of Plesiometa argyra (Araneae, Tetragnathidae) when parasitized by Hymenoepimecis argyraphaga (Hymenoptera, Ichneumonidae) SO JOURNAL OF ARACHNOLOGY LA English DT Article DE parasite; manipulation of host behavior; orb construction behavior; Plesiometa; Hymenoepimecis ID NEPHILA-CLAVIPES ARANEAE; SPIDERS ARANEAE; MANIPULATION; CONSTRUCTION; PHYLOGENY; ARANEIDAE AB On the evening that it will kill its host, the orb-weaving spider Plesiometa argyra, the larva of the ichneumonid wasp Hymenoepimecis argyraphaga induces the spider to perform highly stereotyped construction behavior and build an otherwise unique "cocoon web" that is particularly well-designed to support the wasp larva's cocoon. Cocoon web construction behavior is nearly identical with the early steps in one subroutine of normal orb construction, and is repeated over and over. Usually all other normal orb construction behavior patterns are completely or nearly completely repressed. Experimental removal of the larva one or a few hours before cocoon construction would normally occur is sometimes followed by nearly normal cocoon web construction, and sometimes by construction of other highly altered web designs. The mechanism by which the larva induces these changes in the spider's behavior is thus apparently a fast acting chemical, with effects that are manifested gradually. Partial recovery of orb designs sometimes occurred several days later. C1 Smithsonian Trop Res Inst, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Smithsonian Trop Res Inst, Ciudad Univ, San Jose, Costa Rica. NR 33 TC 40 Z9 45 U1 7 U2 97 PU AMER ARACHNOLOGICAL SOC PI NEW YORK PA C/O NORMAN I PLATNICK, AMER MUSEUM NATURAL HISTORY, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024 USA SN 0161-8202 J9 J ARACHNOL JI J. Arachnol. PY 2001 VL 29 IS 3 BP 354 EP 366 DI 10.1636/0161-8202(2001)029[0354:UTIWAB]2.0.CO;2 PG 13 WC Entomology SC Entomology GA 508YV UT WOS:000173118100006 ER PT J AU Zeder, MA AF Zeder, MA TI A metrical analysis of a collection of modern goats (Capra hircus aegargus and C. h. hircus) from Iran and Iraq: Implications for the study of caprine domestication SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE domestication; size reduction; demographic profiling; Capra hircus; Near East ID SHEEP AB A critical comparison of two commonly used markers of initial animal domestication, size reduction and demographic profiling, is presented. A metrical analysis of a large collection of modern wild and domestic goats (Capra hircus aegargus and C. h. hircus) from Iran and Iraq clearly demonstrates that sex is by far the most significant factor affecting size in goats. In all post-cranial bones examined, those of males, even the unfused bones of males over 1 year of age, are absolutely larger than the bones of females. Region also plays a significant role in the size of these animals, but domestic status seems to have little impact. Similarly, a re-analysis of archaeological assemblages from Upland Sites the eastern fertile crescent shows no evidence of population-wide size reduction over a period that encompasses the transition from hunting to herding goats in the region, from the Middle Palaeolithic to the Early Neolithic. The apparent rapid reduction in the size of caprines during the early phases of domestication noted in earlier studies is likely attributable to a shift in the sex ratio of the adult breeding population of managed herds towards female domination, plus the differential destruction and loss of the bones of male animals killed at younger ages, as well as biases introduced by standard methodological practices. Building on the earlier work of Hesse, and using the empirical understanding of the factors influencing size in modern goats gained in this study, a new approach is proposed that combines both size and long-bone fusion data to construct high resolution, sex-specific age profiles of male and female goats that can be used to detect the hunting to herd management transition which marks the initial stages of the domestication process. Copyright 2001 Academic Press C1 Smithsonian Inst, Amer Museum Nat Hist, Archaeobiology Program, Washington, DC 20560 USA. RP Zeder, MA (reprint author), Smithsonian Inst, Amer Museum Nat Hist, Archaeobiology Program, 10th & Constitution Ave NW, Washington, DC 20560 USA. NR 41 TC 56 Z9 60 U1 0 U2 15 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD JAN PY 2001 VL 28 IS 1 BP 61 EP 79 DI 10.1006/jasc.1999.0555 PG 19 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 398UW UT WOS:000166775700006 ER PT J AU Coss, CA Robledo, JAF Ruiz, GM Vasta, GR AF Coss, CA Robledo, JAF Ruiz, GM Vasta, GR TI Description of Perkinsus andrewsi n. sp isolated from the baltic clam (Macoma balthica) by characterization of the ribosomal RNA locus, and development of a species-specific PCR-based diagnostic assay SO JOURNAL OF EUKARYOTIC MICROBIOLOGY LA English DT Article DE Crassostrea virginica; diagnostic assay; ITS; Mercenaria mercenaria; NTS; PCR; SSU ID INTERNAL TRANSCRIBED SPACERS; IN-VITRO CULTURE; EASTERN OYSTER; CRASSOSTREA-VIRGINICA; RUDITAPES-PHILIPPINARUM; NONTRANSCRIBED SPACER; NUCLEOTIDE-SEQUENCE; PHYLUM APICOMPLEXA; MARINUS DISEASE; PARASITE AB A Perkinsus species was isolated from the baltic clam Macoma balthica and an in vitro culture established under conditions described for P. marinus. As reported previously, morphological features remarkable enough to clearly indicate that this isolate is a distinct Perkinsus species were lacking. In this study, regions of the rRNA locus (NTS, 18S, ITS1, 5.8S, and ITS2) of this isolate were cloned, sequenced, and compared by alignment with those available for other Perkinsus species and isolates. Sequence data from the rRNA locus and species-specific PCR assays indicated not only that Perkinsus sp. from M. balthica was not P. marinus, but it was different from P. atlanticus and P. olseni. The degree of difference was comparable to or greater than differences between accepted Pr Perkinsus species. In particular, NTS sequence and length were dramatically different From that of P. marinus and P. atlanticus. Therefore. we formally propose to designate the Perkinsus sp. from M. balthica as a separate species. P. andrewsi n. sp. Primers based on P. andrewsi NTS sequence were used to develop a PCR-based diagnostic assay that was validated for species-specificity and sensitivity. PCR-based assays specific for either P. andrewsi or P. marinus were used to test for their presence in bivalve species sympatric to M. balthica. Although isolated from M. balthica. P. andrewsi was also detected in the oyster Crassostrea virginica and clams Macoma mitchelli and Mercenaria mercenaria, and could coexist with P. marinus in all four bivalve species tested. C1 Univ Maryland, Ctr Marine Biotechnol, Inst Biotechnol, Baltimore, MD 21202 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Vasta, GR (reprint author), Univ Maryland, Ctr Marine Biotechnol, Inst Biotechnol, 600 E Lombard St, Baltimore, MD 21202 USA. OI Ruiz, Gregory/0000-0003-2499-441X NR 60 TC 65 Z9 67 U1 1 U2 7 PU SOC PROTOZOOLOGISTS PI LAWRENCE PA 810 E 10TH ST, LAWRENCE, KS 66044 USA SN 1066-5234 J9 J EUKARYOT MICROBIOL JI J. Eukaryot. Microbiol. PD JAN-FEB PY 2001 VL 48 IS 1 BP 52 EP 61 DI 10.1111/j.1550-7408.2001.tb00415.x PG 10 WC Microbiology SC Microbiology GA 407TG UT WOS:000167286400009 PM 11249193 ER PT J AU Dutro, JT Yochelson, EL AF Dutro, JT Yochelson, EL TI Memorial - G. Arthur Cooper 1902-1999 SO JOURNAL OF PALEONTOLOGY LA English DT Biographical-Item C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Dutro, JT (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD JAN PY 2001 VL 75 IS 1 BP 222 EP 223 PG 2 WC Paleontology SC Paleontology GA 400EN UT WOS:000166859400016 ER PT J AU Good, EM AF Good, EM TI Makers of the piano, vol 2, 1820-1860 SO JOURNAL OF THE AMERICAN MUSICAL INSTRUMENT SOCIETY LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Good, EM (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER MUSIC INSTRUMENT SOC PI HEMPSTEAD PA MUSIC DEPT, EMILY LOWE HALL 112 HOFSTRA UNIVERSITY, HEMPSTEAD, NY 11362 USA SN 0362-3300 J9 J AM MUSIC INSTRUM S JI J. Am. Music. Instrum. Soc. PY 2001 VL 27 BP 198 EP 200 PG 3 WC Music SC Music GA 488LE UT WOS:000171936000009 ER PT J AU Ireland, RR Robinson, H AF Ireland, RR Robinson, H TI Taxonomic status of Ditrichum ambiguum and D-tortuloides SO JOURNAL OF THE HATTORI BOTANICAL LABORATORY LA English DT Article AB Ditrichum tortuloides Grout from the eastern United States has been considered a synonym of D. ambiguum Best from the western part of North America, however, the present study reveals they are closely related, but distinct species. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. RP Ireland, RR (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. NR 15 TC 0 Z9 0 U1 0 U2 0 PU HATTORI BOTANICAL LABORATORY PI NIYAZAKI-KEN PA OBI, NICHINAN-SHI, NIYAZAKI-KEN, 889-2535, JAPAN SN 0073-0912 J9 J HATTORI BOT LAB JI J. Hattori Bot. Lab. PY 2001 IS 91 BP 277 EP 287 PG 11 WC Plant Sciences SC Plant Sciences GA 514TB UT WOS:000173456200007 ER PT J AU Schultz, TR Engel, MS Ascher, JS AF Schultz, TR Engel, MS Ascher, JS TI Evidence for the origin of eusociality in the corbiculate bees (Hymenoptera : Apidae) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article ID MAJOR OPSIN; HYMENOPTERA; EVOLUTION; SEQUENCES; APOIDEA; TREES AB Several recent phylogenetic analyses of separate morphological, molecular, and paleontological data sets have addressed evolutionary relationships among the tribes of corbiculate bees (Apidae: Apini, Bombini, Euglossini, and Meliponini). These analyses appear to disagree in their implications about the evolution of eusociality within this group. Whereas morphological and paleontological data strongly support the classical hypothesis of a single origin of general eusociality and a single origin of advanced eusociality, some authors have suggested that molecular data strongly contradict this view, and instead support independent, parallel origins of advanced eusociality or, alternatively, evolutionary reversals to solitary behavior from a eusocial ancestor common to all corbiculate bees. In order to reconcile this conflict between morphology and molecules, these authors have suggested that the morphological data may be flawed. We briefly review the evidence for this disagreement between morphological and molecular data and conclude that it is exaggerated; we also find the various criticisms of the morphological data unpersuasive. By any standard phylogenetic measure, three of four molecular data sets are ambiguous in their support of alternate hypotheses regarding eusocial evolution, whereas morphological, paleontological, and recent ethological data are unequivocal. Judged in its entirety, then, the available evidence continues to support Darwin's null hypothesis of (Euglossini + (Bombini + (Apini + Meliponini))) and single origins for both general and advanced eusocial behavior in the corbiculate bees. C1 Natl Museum Nat Hist, Dept Systemat Biol, Smithsonian Inst, Washington, DC 20560 USA. Univ Kansas, Div Entomol, Museum Nat Hist, Lawrence, KS 66045 USA. Univ Kansas, Biodivers Res Ctr, Lawrence, KS 66045 USA. Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. Cornell Univ, Dept Entomol, Ithaca, NY 14853 USA. RP Schultz, TR (reprint author), Natl Museum Nat Hist, Dept Systemat Biol, Smithsonian Inst, MRC 188, Washington, DC 20560 USA. RI Engel, Michael/C-5461-2012; Ascher, John/D-1554-2014 OI Engel, Michael/0000-0003-3067-077X; NR 26 TC 30 Z9 32 U1 1 U2 9 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD JAN PY 2001 VL 74 IS 1 BP 10 EP 16 PG 7 WC Entomology SC Entomology GA 487GA UT WOS:000171864200002 ER PT J AU Poulin, B Lefebvre, G Ibanez, R Jaramillo, C Hernandez, C Rand, AS AF Poulin, B Lefebvre, G Ibanez, R Jaramillo, C Hernandez, C Rand, AS TI Avian predation upon lizards and frogs in a neotropical forest understorey SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Anolis lizards; avian diet; Eleutherodactylus frogs; neotropical birds; Panama; predator-prey interactions; social foraging; tartar emetic ID POISON FROGS; FOOD-WEB; ANOLINE LIZARDS; BIRDS; DIET; WOODCREEPERS; ECOLOGY; PANAMA; SIZE AB Although tropical forest birds are known to prey upon small lizards and frogs, no study has documented the attributes of vertebrate-eating birds or whether birds prey opportunistically on the different elements of the herpetofauna within tropical communities. This study is based on a 14-mo investigation on avian diet, supplemented with a 3-y census of frogs and a 1-y census of lizards in a humid forest of central Panama. From 91 bird species, 1086 regurgitates were collected, in which were found 75 lizards and 53 frogs. Over 50% of the common, primarily insectivorous bird species preyed upon lizards or frogs, with a mean frequency of 0.26 prey/sample. These birds (22 species, nine families) foraged on various substrates from different strata of the forest, fed on invertebrates averaging from 3.3 to 17.2 mm in length, weighed from 11 to 195 g, and had bill lengths that varied from 12.2 to 49.8 mm. Based on a logistic regression analysis, intensity of foraging at army-ant swarms was the variable that best explained the likelihood that a bird species preyed upon lizards, leading to a classification that was 91% correct. In contrast, bill length and body length classified correctly 88% of the frog-eating birds, which showed a fairly constant 1:7 bill length/body length ratio (as opposed to a mean but highly variable 1:10 ratio in other species). A multiple regression analysis showed that seasonal variation in intensity of lizard predation was positively related to arthropod abundance except during the breeding season when lizard intake decreased, presumably because nesting birds did not follow ant swarms. Intensity of frog predation correlated with frog abundance over time, the latter being inversely related to arthropod availability. Ninety-seven per cent of all lizards and frogs identified in the diet samples (n = 105) were from two genera, Anolis and Eleutheradactylus, respectively. Prey size distribution in the regurgitates suggested an optimal prey size of 33.5 mm snout-vent length (SVL) for lizards and 14.5 mm SVL for frogs. Birds preyed opportunistically on the different Anolis species, but almost exclusively upon juvenile individuals. Abundances of the different Eleutherodactylus species correlated with their predation rates, but these frogs represented only 10% of all the frogs observed during the censuses. The two most common local anurans, Colostethus flotator and Bufo typhonius, were not taken by any bird species. C1 Smithsonian Trop Res Inst, Ancon 2072, Panama. RP Poulin, B (reprint author), Stn Biol Tour Valat, F-13200 Arles, France. NR 46 TC 41 Z9 45 U1 1 U2 23 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD JAN PY 2001 VL 17 BP 21 EP 40 DI 10.1017/S026646740100102X PN 1 PG 20 WC Ecology SC Environmental Sciences & Ecology GA 402NF UT WOS:000166994400002 ER PT J AU Svenning, JC AF Svenning, JC TI Environmental heterogeneity, recruitment limitation and the mesoscale distribution of palms in a tropical montane rain forest (Maquipucuna, Ecuador) SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Andes; Arecaceae; dispersal limitation; logistic regression; spatial autocorrelation; species-environment relationships ID LANDSCAPE-SCALE DISTRIBUTIONS; SPECIES DISTRIBUTIONS; LOGISTIC-REGRESSION; PLANT-POPULATIONS; AMAZONIAN ECUADOR; ARBORESCENT PALMS; SEED DISPERSAL; TREEFALL GAPS; CLOUD FOREST; COSTA-RICA AB The study presented here investigated the importance of environmental heterogeneity and clumping for the mesoscale distribution patterns of five palm species in old-growth Andean forest (Maquipucuna, Ecuador). Seedlings, juveniles and adults were recorded in 167 plots located throughout the 3-km X 3-km study area. Mountain (Cerro Sosa or Cerro Sta. Lucia), altitude, aspect, topographic-edaphic conditions and forest structure were also recorded. The following questions were investigated: (1) Are the distributions related to environmental heterogeneity? (2) Are the distribution patterns consistent with severe recruitment limitation? The distribution patterns of four species were related to environmental heterogeneity, especially to that created by the mountainous landscape itself, and at least four of the five species also exhibited strong clumping that was clearly linked to spatially restricted recruitment and could not be explained by the environmental parameters. Thus, both niche specialization and recruitment limitation probably play important roles in Andean palm community ecology. Consistent differences among the two mountains in forest structure and the frequency of certain palm stages most likely reflected extractivism. C1 Aarhus Univ, Dept Systemat Bot, Herbarium AAU, DK-8000 Aarhus C, Denmark. RP Svenning, JC (reprint author), Smithsonian Trop Res Inst, Unit 0948,APO AA, Miami, FL 34002 USA. RI Svenning, Jens-Christian/C-8977-2012 OI Svenning, Jens-Christian/0000-0002-3415-0862 NR 75 TC 50 Z9 59 U1 0 U2 11 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD JAN PY 2001 VL 17 BP 97 EP 113 DI 10.1017/S0266467401001067 PN 1 PG 17 WC Ecology SC Environmental Sciences & Ecology GA 402NF UT WOS:000166994400006 ER PT J AU Raymond, JT Garner, MM Nordhausen, RW Jacobson, ER AF Raymond, JT Garner, MM Nordhausen, RW Jacobson, ER TI A disease resembling inclusion body disease of boid snakes in captive palm vipers (Bothriechis marchi) SO JOURNAL OF VETERINARY DIAGNOSTIC INVESTIGATION LA English DT Article AB Between April 1998 and June 1999, 8 palm vipers (Bothriechis marchi) were diagnosed with a disease similar to inclusion body disease (IBD) of boids. Six palm vipers were captive bred, and 2 were wild caught. All of the vipers were adults at the time of death. Three palm vipers were found dead with no premonitory clinical signs, and 5 had anorexia plus possibly 1 of the following clinical signs: regurgitation, paresis, and dehydration. Histologically, all snakes had intracytoplasmic, round to oval, single to multiple eosinophilic inclusion bodies in hepatocytes and renal tubular epithelial cells. Inclusion bodies were distributed among other organs with varying frequency. Common concurrent histologic lesions were urate nephrosis, septic thrombi, and hepatocellular degeneration. Ultrastructurally, inclusions had features similar to inclusions in boid snakes with IBD. C1 Smithsonian Natl Zool Pk, Washington, DC 20008 USA. Univ Calif Davis, Sch Vet Med, Calif Vet Diagnost Lab, Davis, CA 95616 USA. Univ Florida, Dept Small Anim Clin Sci, Gainesville, FL 32610 USA. RP Raymond, JT (reprint author), NW Zoopath, 18210 Waverly Dr, Snohomish, WA 98296 USA. NR 9 TC 12 Z9 12 U1 1 U2 3 PU AMER ASSOC VETERINARY LABORATORY DIAGNOSTICIANS INC PI TURLOCK PA PO BOX 1522, TURLOCK, CA 95381 USA SN 1040-6387 J9 J VET DIAGN INVEST JI J. Vet. Diagn. Invest. PD JAN PY 2001 VL 13 IS 1 BP 82 EP 86 PG 5 WC Veterinary Sciences SC Veterinary Sciences GA 458XP UT WOS:000170221000017 PM 11243371 ER PT J AU Nichols, DK Lamirande, EW Pessier, AP Longcore, JE AF Nichols, DK Lamirande, EW Pessier, AP Longcore, JE TI Experimental transmission of cutaneous chytridiomycosis in dendrobatid frogs SO JOURNAL OF WILDLIFE DISEASES LA English DT Article DE Batrachochytrium dendrobatidis; chytrid; cutaneous chytridiomycosis; Dendrobates auratus; Dendrobates tinctorius; experimental infection; fungus; poison dart frog AB In a series of three experiments during March-October, 1998, two species of captive-bred poison dart frogs (Dendrobates tinctorius and D. auratus) were exposed to Batrachochytrium dendrobatidis, a recently-described chytridiomycete fungus (chytrid) that was originally isolated from a blue poison dart frog (D. azureus). All frogs exposed to the chytrids developed a fatal skin disease, whereas none of the control frogs developed skin lesions. The most consistent clinical sign in chytrid-exposed frogs was excessive shedding of skin. Gross lesions were subtle, usually affected the legs and ventrum, and consisted of mild skin thickening and discoloration. Microscopic examination of shed skin pieces and/or skin imprints demonstrated the presence of chytrids and was used for ante mortem and post mortem confirmation of chytrid infection. Histologically, there was epidermal hyperkeratosis, hyperplasia, and hypertrophy associated with low to moderate numbers of chytrids in the keratinized layers. These experiments demonstrated that Batrachochytrium dendrobatidis can be a fatal pathogen in poison dart frogs. The experimentally-induced disease in these frogs resembled cases of cutaneous chytridiomycosis that have recently been described in several other species of captive and wild amphibians. C1 Smithsonian Inst, Natl Zool Pk, Dept Pathol, Washington, DC 20008 USA. Univ Maine, Dept Biol Sci, Orono, ME 04469 USA. RP Nichols, DK (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Pathol, 3000 Connecticut Ave NW, Washington, DC 20008 USA. NR 12 TC 112 Z9 124 U1 5 U2 35 PU WILDLIFE DISEASE ASSN, INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 0090-3558 J9 J WILDLIFE DIS JI J. Wildl. Dis. PD JAN PY 2001 VL 37 IS 1 BP 1 EP 11 PG 11 WC Veterinary Sciences SC Veterinary Sciences GA 402WR UT WOS:000167011600001 PM 11272482 ER PT J AU Kalfatovic, MR AF Kalfatovic, MR TI Ed Ruscha. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC 20560 USA. RP Kalfatovic, MR (reprint author), Smithsonian Inst Lib, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JAN PY 2001 VL 126 IS 1 BP 96 EP 96 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 391XH UT WOS:000166381200041 ER PT S AU Noel, S Burrows, JP Bovensmann, H Frerick, J Chance, KV Goede, AHP Muller, C AF Noel, S Burrows, JP Bovensmann, H Frerick, J Chance, KV Goede, AHP Muller, C BE Debus, A Rummel, JD Horneck, G Rettberg, P TI Atmospheric trace gas sounding with SCIAMACHY SO LIFE SCIENCES: PLANETARY PROTECTION; OZONE AND UVB RADIATION EFFECTS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT F3 4/F3 6 Symposium of COSPAR Scientific Commission F held at the 32nd COSPAR Scientific Meeting CY JUL, 1998 CL NAGOYA, JAPAN SP Ctr Natl Etudes Spatiales, Natl Aeronaut & Space Adm, Comm Space Res, World Meteorol Org, Eurpean Comm, Wolrd Climate Res Programme, Stratospher process & Role Climate ID TROPOSPHERIC OZONE; SATELLITE DATA; PROFILES; GOME; ALGORITHM AB SCIAMACHY (Scanning Imaging Absorption Spectrometer for Atmospheric CHartographY) is a contribution to the ENVISAT-1 satellite, which is to be launched in late 2000, The SCIAMACHY instrument is designed to measure sunlight transmitted, reflected and scattered by the Earth's atmosphere or surface. The instrument measures simultaneously from the UV to the NIR spectral spectral region (240 - 2380 nm). Observations are made in alternate nadir and limb viewing geometries and also for solar sunrise and lunar moonrise occultation. inversion of the SCIAMACHY measurements will provide the following: the amount and distributions of some important trace gases O-3, BrO, OClO, ClO, SO2, H2CO, NO2, CO, CO2, CH4, H2O, N2O, p, T, aerosol, and radiation flux profiles, cloud cover and cloud top height. Combination of the near simultaneous limb and nadir observations enables the tropospheric column amounts of O-3, NO2, CO, CH4, H2O, N2O, SO2, and H2CO to be detected. SCIAMACHY will provide new insight into the global behaviour of the troposphere and the stratosphere. (C) 2001 COSPAR. Published by Elsevier Science Ltd. All rights reserved. C1 Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. SRON Ruimetonderzoek, NL-3584 Utrecht, Netherlands. Inst Aeron Spatiale Belgique, BIRA, B-1180 Brussels, Belgium. RP Noel, S (reprint author), Univ Bremen, Inst Environm Phys, FB 1, D-28334 Bremen, Germany. RI Bovensmann, Heinrich/P-4135-2016; Burrows, John/B-6199-2014 OI Bovensmann, Heinrich/0000-0001-8882-4108; Burrows, John/0000-0002-6821-5580 NR 23 TC 0 Z9 0 U1 1 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0273-1177 J9 ADV SPACE RES PY 2001 VL 26 IS 12 BP 1949 EP 1954 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BS43X UT WOS:000169859200007 ER PT B AU van Ballegooijen, AA Mackay, DH AF van Ballegooijen, AA Mackay, DH BE Mathys, G Solanki, SK Wickramasinghe, DT TI Theory of solar chromospheric and coronal magnetic fields SO MAGNETIC FIELDS ACROSS THE HERTZSPRUNG-RUSSELL DIAGRAM SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Magnetic Fields across the Hertzsprung-Russell Diagram CY JAN 15-19, 2001 CL SANTIAGO, CHILE SP European SO Observ, Cerro Tololo Inter Amer Observ, Univ Catolica Norte ID ACTIVE-REGION; FILAMENT CHANNELS; QUIESCENT PROMINENCES; ELECTRIC CURRENTS; HELICAL STRUCTURE; MASS EJECTIONS; FLUX TRANSPORT; DELTA-GROUP; MODEL; STABILITY AB Magnetic fields play an important role in the structure and dynamics of the solar chromosphere and corona. Here we focus on the strongly sheared and/or helical magnetic fields observed in solar active regions and in filament channels. We review recent observations and models of such non-potential magnetic structures. Helical fields are believed to be formed as a result of the emergence of twisted fields from below the photosphere and the subsequent transport of magnetic flux by diffusion and differential rotation. The diffusion leads to flux cancellation in the photosphere and associated reconnection of magnetic field lines in the corona. Recent models including such flux cancellation are presented. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van Ballegooijen, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 54 TC 0 Z9 0 U1 0 U2 3 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-088-9 J9 ASTR SOC P PY 2001 VL 248 BP 105 EP 114 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU54W UT WOS:000176291300012 ER PT B AU Saar, S Brandenburg, A AF Saar, S Brandenburg, A BE Mathys, G Solanki, SK Wickramasinghe, DT TI Further analysis of stellar magnetic cycle periods SO MAGNETIC FIELDS ACROSS THE HERTZSPRUNG-RUSSELL DIAGRAM SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Magnetic Fields across the Hertzsprung-Russell Diagram CY JAN 15-19, 2001 CL SANTIAGO, CHILE SP European SO Observ, Cerro Tololo Inter Amer Observ, Univ Catolica Norte ID MAIN-SEQUENCE STARS; DIFFERENTIAL ROTATION; TIME EVOLUTION; CLOSE BINARIES; DYNAMO; MODULATION AB We further investigate relationships between activity cycle periods in cool stars and rotation to include new cycle data, and explore different parameterizations of the problem. We find that relations between cycle and rotational frequencies (w(cyc) vs. Omega) and between their ratio and the inverse Rossby number (w(cyc)/Omega vs. Ro(-1)) show many similarities, including three branches and similar rms scatter. We briefly discuss some implications for dynamo models. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Saar, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 19 TC 3 Z9 3 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-088-9 J9 ASTR SOC P PY 2001 VL 248 BP 231 EP 234 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU54W UT WOS:000176291300034 ER PT B AU Hussain, GAJ van Ballegooijen, AA Jardine, M AF Hussain, GAJ van Ballegooijen, AA Jardine, M BE Mathys, G Solanki, SK Wickramasinghe, DT TI Modelling the coronal topology of late-type stars SO MAGNETIC FIELDS ACROSS THE HERTZSPRUNG-RUSSELL DIAGRAM SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Workshop on Magnetic Fields across the Hertzsprung-Russell Diagram CY JAN 15-19, 2001 CL SANTIAGO, CHILE SP European SO Observ, Cerro Tololo Inter Amer Observ, Univ Catolica Norte ID AB AB Surface magnetic field models for AB Doradus are obtained using a technique based on Zeeman Doppler imaging. This technique allows us to model both potential fields as well as currents. The surface field maps presented here show a very strong non-potential component near the visible pole. We show how the coronal topology of the star can be modeled by extrapolating these surface maps. Our coronal field models show the presence of both open and closed field lines, with closed loops extending out beyond the equatorial co-rotation radius. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS16, Cambridge, MA 02138 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-088-9 J9 ASTR SOC P PY 2001 VL 248 BP 263 EP 266 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU54W UT WOS:000176291300042 ER PT J AU Bogdan, D Monfort, SL AF Bogdan, D Monfort, SL TI Faecal oestrogen and progesterone profiles in breeding and non-breeding female North American porcupine (Erethizon dorsatum) SO MAMMALIA LA English DT Article DE porcupine; faecal steroids; progestagens; oestrogens; reproduction ID MONITORING OVARIAN-FUNCTION; FECES; REPRODUCTION; METABOLITES; PREGNANCY; EXCRETION; URINARY; RATES AB A radioimmunoassay was validated to measure faecal oestrogen and progesterone metabolites in captive female North American porcupines (Erethizon dorsatum) (n = 5) for a period of between 261-393 days. Females housed alone (n = 3) exhibited fluctuations in faecal oestrogens indicative of follicular activity yet these solitary females did not ovulate spontaneously. Breeding females (n = 2) appeared to experience pseudopregnancy lasting for approximately 87 and 112 days. In the single successful birth, gestation was 135 days. Faecal progestagen concentrations in breeding females were twice that of non-breeding females, however, occasional overlap between pregnant and non-pregnant hormone concentrations precluded the use of faecal steroids as an index of pregnancy status. These preliminary data suggest that non invasive faecal steroid monitoring is a useful tool for evaluating longitudinal reproductive-endocrine rhythms in porcupines. C1 Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA 22630 USA. CUNY Queens Coll, Dept Biol, Flushing, NY 11367 USA. RP Monfort, SL (reprint author), Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA 22630 USA. NR 23 TC 1 Z9 2 U1 2 U2 9 PU MUSEUM NAT HIST NATURELLE PI PARIS PA SERVICE PUBLICATIONS SCIENTIFIQUES, 57 RUE CUVIER, 75005 PARIS, FRANCE SN 0025-1461 J9 MAMMALIA JI Mammalia PY 2001 VL 65 IS 1 BP 73 EP 81 DI 10.1515/mamm.2001.65.1.73 PG 9 WC Zoology SC Zoology GA 422PW UT WOS:000168128600007 ER PT J AU Wellington, GM Robertson, DR AF Wellington, GM Robertson, DR TI Variation in larval life-history traits among reef fishes across the Isthmus of Panama SO MARINE BIOLOGY LA English DT Article ID GREAT-BARRIER-REEF; DAMSELFISHES POMACENTRIDAE; POPULATION-STRUCTURE; REGIONAL DIFFERENCES; HABITAT SELECTION; EASTERN PACIFIC; RECRUITMENT; SETTLEMENT; PATTERNS; DURATION AB We tested the hypothesis that regional differences in oceanic productivity have led to the evolution of predictable patterns of regional variation in life-history traits of pelagic larvae of tropical reef fishes. To do so we compared larval traits (egg and hatchling size, larval growth rate and duration, and size at settlement) among closely related reef fishes from the Atlantic and Pacific coasts of the Isthmus of Panama. This comparison provides a control for phylogenetic effects because those regions shared a common fauna prior to the rise of the Isthmus similar to3.5 million years ago, subsequent to which each fauna evolved independently under a very different productivity regime. We measured larval traits of 12 benthic-spawning damselfishes (Pomacentridae: Abudeduf, Chromis and Stegastes) and 13 pelagic-spawning wrasses (Labridae: Bodianus, Halichoeres, and Thalassoma). These included members of each genus on each side of the Isthmus and four sets of transisthmian sister species of pomacentrids. Among the pomacentrids we found consistent transisthmian differences in hatchling size, but not in other larval traits. Essentially the reverse pattern occurred among the labrids - larval growth and duration differed consistently among congeners in the two regions, but without consistent differences in hatchling size or size at settlement. Neither relationship is predicted by the regional-productivity hypothesis. Most of the differences were quite small. Stronger phylogenetic effects on larval traits (inter- and intrageneric variation within regions) occur in both families and evidently overwhelm any effect of regional variation in productivity. Reassessment of data that takes into account such phylogenetic effects questions previous conclusions about the existence of regional differences in larval traits among damselfishes in the West Pacific and the Carribean. C1 Univ Houston, Dept Biol & Biochem, Program Ecol & Evolut Biol, Houston, TX 77204 USA. Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Wellington, GM (reprint author), Univ Houston, Dept Biol & Biochem, Program Ecol & Evolut Biol, Houston, TX 77204 USA. NR 54 TC 20 Z9 20 U1 2 U2 9 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD JAN PY 2001 VL 138 IS 1 BP 11 EP 22 DI 10.1007/s002270000449 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 398CT UT WOS:000166738900002 ER PT J AU Wonham, MJ Walton, WC Ruiz, GM Frese, AM Galil, BS AF Wonham, MJ Walton, WC Ruiz, GM Frese, AM Galil, BS TI Going to the source: role of the invasion pathway in determining potential invaders SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE ballast-water transport; nonindigenous species; plankton; invasion success; risk reduction; mid-ocean exchange; shipping ID SHIPS BALLAST WATER; BIOLOGICAL INVASIONS; MARINE ORGANISMS; TRANSPORT; DISPERSAL; OCEAN; TANKS AB Biological invasions are an increasing agent of change in aquatic systems, and ballast-water transfer in ships is a leading pathway of these invasions. During sequential stages of ballast transfer (uptake, transport, and release), the density and diversity of the plankton assemblage is selectively filtered, determining the pool of potential invaders. Understanding taxon-specific patterns of mortality along the invasion pathway is key to understanding and predicting successful invasions. We quantified taxon-specific trends in plankton mortality during a 16 d trans-Atlantic ballast water voyage. In the ballast tanks, we collected a miminum of 50 live taxa. Over 50 % of taxa and > 98% of organisms collected in initial samples were not detected at the end of the voyage. No ballasted organisms survived experimental transfer to coastal harbor water. We suggest that the invasion success of a particular taxon may be predicted both by high density at the end of a voyage (which is comparatively easy to measure) and by low mortality during a voyage (which may indicate good body condition, but is harder to measure). These 2 predictors were not, however, correlated across taxa. Mid-ocean exchange, the most widely used method for reducing ballast-mediated invasion risk, alters the pool of potential invaders. In an experimental test of mid-ocean exchange, 93 to 100 % of the coastal water and 80 to 100 % of the coastal organisms were removed. However, the total density and diversity of plankton in the ballast tanks increased significantly following exchange and in laboratory experiments ocean water was not lethal to coastal organisms. C1 Williams Coll, Mystic Seaport Maritime Studies Program, Mystic, CT 06355 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Maryland, Horn Point Environm Lab, Cambridge, MD 21613 USA. Israel Oceanog & Limnol Res, Haifa, Israel. Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA. RP Wonham, MJ (reprint author), Univ Washington, Dept Zool, POB 351800, Seattle, WA 98195 USA. EM mwonham@u.washington.edu OI Ruiz, Gregory/0000-0003-2499-441X NR 41 TC 106 Z9 112 U1 5 U2 25 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2001 VL 215 BP 1 EP 12 DI 10.3354/meps215001 PG 12 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 450JX UT WOS:000169739900001 ER PT J AU Laist, DW Knowlton, AR Mead, JG Collet, AS Podesta, M AF Laist, DW Knowlton, AR Mead, JG Collet, AS Podesta, M TI Collisions between ships and whales SO MARINE MAMMAL SCIENCE LA English DT Article DE mortality strandings; ship collisions; species conservation; right whales ID NORTH-ATLANTIC; EUBALAENA-GLACIALIS AB Although collisions with motorized ships are a recognized source of whale mortality, little has been done to compile information on the frequency of their occurrence or contributing factors. We searched historical records and computerized stranding databases for evidence of ship strikes involving great whales (i.e., baleen whales and the sperm whale). Historical records suggest that ship strikes fatal to whales first occurred late in the 1800s as ships began to reach speeds of 13-15 kn, remained infrequent until about 1950, and then increased during the 1950s-1970s as the number and speed of ships increased. Of 11 species known to be hit by ships, fin whales (Balaenoptera physalus) are struck most frequently; right whales (Eubalaena glacialis and E. australis), humpback whales (Megaptera novaeangliae), sperm whales (Physeter catodon), and gray whales (Eschrichtius robustus) are hit commonly. In some areas, one-third of all fin whale and right whale strandings appear to involve ship strikes. To assess contributing factors, we compiled descriptions of 58 collisions. They indicate that all sizes and types of vessels can hit whales; most lethal or severe injuries are caused by ships 80 m or longer; whales usually are not seen beforehand or are seen too late to be avoided; and most lethal or severe injuries involve ships travelling 14 kn or faster. Ship strikes can significantly affect small populations of whales, such as northern right whales in the western North Atlantic. In areas where special caution is needed to avoid such events, measures to reduce the vessel speed below 14 kn may be beneficial. C1 Marine Mammal Commiss, Bethesda, MD 20814 USA. New England Aquarium, Right Whale Res, Boston, MA 02110 USA. Smithsonian Inst, Div Mammals, Natl Museum Nat Hist, Washington, DC 20560 USA. Ctr Res Marine Mammals, F-17000 La Rochelle, France. Milano Museum Nat Hist, I-20121 Milan, Italy. RP Laist, DW (reprint author), Marine Mammal Commiss, 4340 EW Highway, Bethesda, MD 20814 USA. NR 54 TC 158 Z9 184 U1 11 U2 88 PU SOC MARINE MAMMALOGY PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 0824-0469 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD JAN PY 2001 VL 17 IS 1 BP 35 EP 75 DI 10.1111/j.1748-7692.2001.tb00980.x PG 41 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 383ML UT WOS:000165886400002 ER PT J AU Cameron, AGW AF Cameron, AGW TI From interstellar gas to the Earth-Moon system SO METEORITICS & PLANETARY SCIENCE LA English DT Article; Proceedings Paper CT Conference on Planetary Impact Events and Their Consequences on Earth (PIECE-99) CY SEP, 1999 CL YAMAGUCHI, JAPAN ID SINGLE-IMPACT HYPOTHESIS; STAR-FORMATION; CLOUD CORES; ORIGIN; SIMULATIONS; DISKS AB This paper reports the current status of my smoothed particle hydrodynamic (SPH) simulations of the formation of the Moon. Since the Moon has recently been found to have been formed approximately 50 Ma after the solar nebula itself was formed, I have placed the lunar formation problem in the entire context of the formation and early evolution of the solar nebula. This set of processes remains controversial, and I have outlined what I believe to be the essential physical processes involved. These start with the formation of short-lived (now extinct) radioactive nuclides in a massive : triggering the collapse of a core supernova. Then follows the probable role of the supernova ejecta In in a molecular cloud to form the solar nebula, and the injection of the radioactivities into the collapsing cloud core. Most of the solar nebula dissipates to form the Sun, and what remains becomes relatively quiescent. Gas drag acting on interstellar grains and the dustballs formed from them, due both to vertical descent to midplane and inward spiralling in midplane, quickly causes growth of the solid materials to form planetesimals. When these bodies reach the kilometer size range and beyond, gravitational forces dominate the accumulation process. The accumulation of the Earth requires of the order of 10(8) years. About half-way through that process the giant impact occurs with the next largest accumulating body near the protoearth. I have been simulating the giant impact using SPH with 100 000 particles. The simulations of three of these runs are depicted in detail with a series of color images. It is shown that conventional accumulation simulations that assume Keplerian orbits and that merge bodies upon collision are misleading because they cannot take account of tidal stripping nor of loss and gain of particles during the accumulation. In addition, the large rotational flattening of the protoearth renders the orbital motions nonkeplerian. The simulations that are shown in detail have been followed for just over a week of real time, and in that time the largest accumulating clump has reached about: half or more of the mass of the Moon and additional clumps have accumulated into bodies in the range of 1 to 20% of a lunar mass. It is important to note that although these runs have given very promising results, the parameter space that could plausibly be associated with the giant impact is not yet adequately explored. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cameron, AGW (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. NR 28 TC 32 Z9 32 U1 2 U2 5 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 0026-1114 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JAN PY 2001 VL 36 IS 1 BP 9 EP 22 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 414EH UT WOS:000167652600003 ER PT J AU Petaev, MI Meibom, A Krot, AN Wood, JA Keil, K AF Petaev, MI Meibom, A Krot, AN Wood, JA Keil, K TI The condensation origin of zoned metal grains in Queen Alexandra Range 94411: Implications for the formation of the Bencubbin-like chondrites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID SOLAR NEBULA; SYSTEMS; BRECCIA AB Thermodynamic analysis of the compositional profiles across large chemically-zoned Fe,Ni metal grains in the Bencubbin-like chondrite Queen Alexandra Range (QUE) 94411 suggests that these grains formed by non-equilibrium gas-solid condensation under variable oxidizing conditions, isolation degree, and Cr depletion factors. The oxidizing conditions must have resulted from the complete vaporization of nebular regions with enhanced dust/gas ratios (similar to 10-40 x solar). Because the origin of each of the metal grains studied requires different condensation parameters (dust/gas ratio, isolation degree, and Cr depletion factor), a high degree of heterogeneity in the formation region of the Bencubbin-like chondrite metal is required. To preserve compositional zoning of the metal grains and prevent their melting and sulfidization, the grains must have been removed from the hot condensation region into cold regions where the accretion of the Bencubbin-like asteroidal body took place. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Hawaii, Hawaii Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. RP Petaev, MI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 32 TC 40 Z9 40 U1 0 U2 3 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 0026-1114 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JAN PY 2001 VL 36 IS 1 BP 93 EP 106 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 414EH UT WOS:000167652600009 ER PT J AU Maldonado, JE Vila, C Wayne, RK AF Maldonado, JE Vila, C Wayne, RK TI Tripartite genetic subdivisions in the ornate shrew (Sorex ornatus) SO MOLECULAR ECOLOGY LA English DT Article DE allozymes; conservation; cytochrome b; mitochondrial DNA; phylogeography; Soricidae ID CYTOCHROME-B GENE; DNA SEQUENCE DATA; MITOCHONDRIAL-DNA; NUCLEOTIDE-SEQUENCES; POPULATION-STRUCTURE; ELECTROPHORETIC DATA; POCKET GOPHERS; ICE AGES; EVOLUTIONARY; SPECIATION AB We examined cytochrome b sequence variation in 251 ornate shrews (Sorex ornatus) from 20 localities distributed throughout their geographical range. Additionally, vagrant (S. vagrans) and montane (S. monticolus) shrews from four localities were used as outgroups. We found 24 haplotypes in ornate shrews from California (USA) and Baja California (Mexico) that differed by 1-31 substitutions in 392 bp of mitochondrial DNA (mtDNA) sequence. In a subset of individuals, we sequenced 699 bp of cytochrome b to better resolve the phylogeographic relationships of populations. The ornate shrew is phylogeographically structured into three haplotype clades representing southern, central and northern localities. Analysis of allozyme variation reveals a similar pattern of variation. Several other small California vertebrates have a similar tripartite pattern of genetic subdivision. We suggest that topographic barriers and expansion and contraction of wetland habitats in the central valley during Pleistocene glacial cycles account for these patterns of genetic variation. Remarkably, the northern ornate shrew clade is phylogenetically clustered with another species of shrew suggesting that it may be a unique lowland form of the vagrant shrew that evolved in parallel to their southern California counterparts. C1 Univ Calif Los Angeles, Dept Organism Biol Ecol & Evolut, Los Angeles, CA 90095 USA. Uppsala Univ, Dept Evolutionary Biol, S-75236 Uppsala, Sweden. RP Maldonado, JE (reprint author), Smithsonian Inst, Natl Zool Pk, Genet Mol Lab, Dept Conservat Biol, 3001 Connecticut Ave NW, Washington, DC 20008 USA. RI Vila, Carles/H-4893-2013 OI Vila, Carles/0000-0002-4206-5246 NR 97 TC 47 Z9 51 U1 0 U2 4 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD JAN PY 2001 VL 10 IS 1 BP 127 EP 147 DI 10.1046/j.1365-294X.2001.01178.x PG 21 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 396QB UT WOS:000166647100013 PM 11251793 ER PT J AU Vandiver, PB AF Vandiver, PB TI Preserving art through the ages SO MRS BULLETIN LA English DT Article C1 Smithsonian Ctr Mat Res & Educ, Suitland, MD 20746 USA. RP Vandiver, PB (reprint author), Smithsonian Ctr Mat Res & Educ, Suitland, MD 20746 USA. NR 11 TC 3 Z9 3 U1 0 U2 0 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DR, WARRENDALE, PA 15086 USA SN 0883-7694 J9 MRS BULL JI MRS Bull. PD JAN PY 2001 VL 26 IS 1 BP 13 EP 18 DI 10.1557/mrs2001.13 PG 6 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA 396UL UT WOS:000166654800014 ER PT J AU Mecklenburg, MF Tumosa, CS AF Mecklenburg, MF Tumosa, CS TI Traditional oil paints: The effects of long-term chemical and mechanical properties on restoration efforts SO MRS BULLETIN LA English DT Article C1 Smithsonian Inst, SCMRE, MSC, Suitland, MD 20746 USA. RP Mecklenburg, MF (reprint author), Smithsonian Inst, SCMRE, MSC, 4210 Silver Hill Rd, Suitland, MD 20746 USA. NR 6 TC 6 Z9 6 U1 1 U2 1 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DR, WARRENDALE, PA 15086 USA SN 0883-7694 J9 MRS BULL JI MRS Bull. PD JAN PY 2001 VL 26 IS 1 BP 51 EP 54 DI 10.1557/mrs2001.19 PG 4 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA 396UL UT WOS:000166654800020 ER PT J AU Lake, S AF Lake, S TI The challenge of preserving modern art: A technical investigation of paints used in selected works by Willem de Kooning and Jackson Pollock SO MRS BULLETIN LA English DT Article C1 Smithsonian Inst, Hirshhorn Museum & Sculpture Garden, Washington, DC 20560 USA. RP Lake, S (reprint author), Smithsonian Inst, Hirshhorn Museum & Sculpture Garden, 7th St & Independence SW, Washington, DC 20560 USA. NR 15 TC 1 Z9 1 U1 0 U2 5 PU MATERIALS RESEARCH SOCIETY PI WARRENDALE PA 506 KEYSTONE DR, WARRENDALE, PA 15086 USA SN 0883-7694 J9 MRS BULL JI MRS Bull. PD JAN PY 2001 VL 26 IS 1 BP 56 EP 60 DI 10.1557/mrs2001.20 PG 5 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA 396UL UT WOS:000166654800021 ER PT B AU Kaaret, P AF Kaaret, P BE Carraminana, A Reimer, O Thompson, DJ TI Massive stars and gamma-ray sources SO NATURE OF UNIDENTIFIED GALACTIC HIGH-ENERGY GAMMA-RAY SOURCES SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Workshop on the Nature of Unidentified Galactic High-Energy Gamma-Ray Sources CY OCT 09-11, 2000 CL INST NACL ASTROFIS, OPT & ELECTR, TONANTZINTLA, MEXICO SP Consejo Nacl Ciencia & Technol HO INST NACL ASTROFIS, OPT & ELECTR DE gamma rays : observations; gamma rays : sources; pulsars : general; stars : individual : 2EG J0635+0521, 3EG J0634+0521, PSR J1259-63, SAX J0635+0533; stars : neutron ID DISCOVERY; PULSAR AB I describe statistical correlations between tracers of Population I objects and EGRET sources, present results from a multiwavelength search of the error box of the unidentified EGRET source in Monoceros, and speculate on a potential new class of gamma-ray emitting objects related to massive stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kaaret, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Reimer, Olaf/A-3117-2013 OI Reimer, Olaf/0000-0001-6953-1385 NR 18 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-0010-3 J9 ASTROPHYS SPACE SC L PY 2001 VL 267 BP 191 EP 196 PG 6 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA BT52H UT WOS:000173242800013 ER PT B AU Slane, P AF Slane, P BE Carraminana, A Reimer, O Thompson, DJ TI Guiding the way to gamma-ray sources: X-ray studies of supernova remnants SO NATURE OF UNIDENTIFIED GALACTIC HIGH-ENERGY GAMMA-RAY SOURCES SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Workshop on the Nature of Unidentified Galactic High-Energy Gamma-Ray Sources CY OCT 09-11, 2000 CL INST NACL ASTROFIS, OPT & ELECTR, TONANTZINTLA, MEXICO SP Consejo Nacl Ciencia & Technol HO INST NACL ASTROFIS, OPT & ELECTR DE supernova remnants; gamma-ray sources ID NONLINEAR SHOCK ACCELERATION; UNIDENTIFIED EGRET SOURCE; SNR RX J1713.7-3946; NEUTRON-STARS; EMISSION; RADIO; SHELL; DISCOVERY; LUMINOSITY; NEBULAE AB Supernova remnants have long been suggested as a class of potential counterparts to unidentified gamma-ray sources. The mechanisms by which such gamma-rays can arise may include emission from a pulsar associated with a remnant, or a variety of processes associated with energetic particles accelerated by the SNR shock. Imaging and spectral observations in the X-ray band can be used to identify properties of the remnants that lead to gamma-ray emission, including the presence of pulsar-driven nebulae, nonthermal X-ray emission from the SNR shells, and the interaction of SNRs with dense surrounding material. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Reimer, Olaf/A-3117-2013 OI Reimer, Olaf/0000-0001-6953-1385 NR 47 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-0010-3 J9 ASTROPHYS SPACE SC L PY 2001 VL 267 BP 227 EP 242 PG 16 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA BT52H UT WOS:000173242800016 ER PT S AU Kalogera, V AF Kalogera, V BE Kouveliotou, C Ventura, J VandenHeuvel, E TI Coalescence rates of compact objects SO NEUTRON STAR - BLACK HOLE CONNECTION SE NATO Science Series II-Mathematics Physics and Chemistry LA English DT Proceedings Paper CT NATO Advanced Study Institute on the Neutron Star - Black Hole Connection CY JUN 07-18, 1999 CL ELOUNDA, GREECE SP NATO Sci Affairs Div ID NEUTRON-STAR BINARIES; PULSAR; ACCRETION; SYSTEM; GALAXY AB Current estimates of the Galactic coalescence rates of close binaries with two compact objects (neutron stars or black holes) are reviewed, in the context of gravitational wave detection. The uncertainties involved in obtaining both theoretical and empirical estimates are discussed as well as empirical ways of obtaining upper limits on the coalescence rate of double neutron star systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kalogera, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vkalogera@cfa.harvard.edu NR 20 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 1568-2609 BN 1-4020-0205-X; 1-4020-0204-1 J9 NATO SCI SER II-MATH PY 2001 VL 567 BP 89 EP 94 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU29N UT WOS:000175586800007 ER PT B AU Tananbaum, H Weisskopf, M AF Tananbaum, H Weisskopf, M BE Inoue, H Kunieda, H TI A general description and current status of the Chandra X-ray Observatory SO NEW CENTURY OF X-RAY ASTRONOMY SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Symposium on New Century of X-Ray Astronomy CY MAR 06-08, 2001 CL YOKOHAMA, JAPAN ID CLUSTER; NEBULA AB The third of NASA's four Great Observatories, the Chandra X-ray Observatory, was launched aboard the Shuttle Columbia on July 23, 1999. Here we describe the principal elements of the Observatory, summarize the mission status, and present selected science highlights. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tananbaum, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 6 Z9 6 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-091-9 J9 ASTR SOC P PY 2001 VL 251 BP 4 EP 9 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU69N UT WOS:000176731500001 ER PT B AU Matsumoto, H Tsuru, TG Matsushita, S Harashima, T Iwamuro, F Maihara, T Kawabe, R AF Matsumoto, H Tsuru, TG Matsushita, S Harashima, T Iwamuro, F Maihara, T Kawabe, R BE Inoue, H Kunieda, H TI Discovery of a candidate for a medium-massive black hole in M82 SO NEW CENTURY OF X-RAY ASTRONOMY SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Symposium on New Century of X-Ray Astronomy CY MAR 06-08, 2001 CL YOKOHAMA, JAPAN AB We present results from X-ray, radio, and infrared observations of the starburst galaxy M82 with the Chandra X-Ray Observatory, the Nobeyarna Millimeter Array, and the SUBARU telescope. We found a strong candidate for a medium-massive black hole (10(3) - 10(6) M.), and a molecular superbubble surrounding the black hole (BH). The kinetic energy of the superbubble is similar to 10(55) ergs, which suggests that all enormous explosion due to starburst activity produced the medium-massive BH and the! superbubble. Based on our observational results, we propose a scenario for the formation of a super-massive BH through a medium-massive BH. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Kyoto Univ, Kyoto, Japan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Tokyo, Tokyo, Japan. RP Matsumoto, H (reprint author), MIT, Ctr Space Res, 77 Massachusetts Ave,NE80-645, Cambridge, MA 02139 USA. NR 9 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-091-9 J9 ASTR SOC P PY 2001 VL 251 BP 60 EP 63 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU69N UT WOS:000176731500011 ER PT B AU Fabbiano, G AF Fabbiano, G BE Inoue, H Kunieda, H TI Observations of galaxies with future X-ray observatories SO NEW CENTURY OF X-RAY ASTRONOMY SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Symposium on New Century of X-Ray Astronomy CY MAR 06-08, 2001 CL YOKOHAMA, JAPAN ID HIGH-RESOLUTION CAMERA; STARBURST GALAXIES; ELLIPTIC GALAXIES; M82; DISCOVERY; REGION; FLOWS; GAS AB Normal galaxies are faint and complex X-ray sources that provide very powerful probes for fundamental astrophysical questions. Examples include: the study of populations of X-ray emitting sources; the study of the entire spectrum of black-hole phenomena; and galaxy formation and evolution in interaction with the surrounding environment. While exciting, all these fields require Chandra sub-arcsecond resolution, and at least comparable spectral capabilities. They also require much large collecting areas. I argue that this is the direction we must plan for future X-ray observatories. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pepi@gcfa.harvard.edu NR 30 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-091-9 J9 ASTR SOC P PY 2001 VL 251 BP 68 EP 73 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU69N UT WOS:000176731500013 ER PT B AU Mukai, K Kallman, T Schlegel, E Bruch, A Handler, G Kemp, J AF Mukai, K Kallman, T Schlegel, E Bruch, A Handler, G Kemp, J BE Inoue, H Kunieda, H TI Chandra HETG observation of the magnetic cataclysmic variable V1223 Sagittarii SO NEW CENTURY OF X-RAY ASTRONOMY SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Symposium on New Century of X-Ray Astronomy CY MAR 06-08, 2001 CL YOKOHAMA, JAPAN ID IRON AB V1223 Sgr is among the brightest magnetic cataclysmic variables in the 1-10 keV band, with a 3.36 hr orbital period and a 745.6 s spin period. Here we report selected results from our Chandra HETG observation, performed on 2000 April 30/May 1. We have detected Kalpha lines of many atomic species in the phase-averaged HETG spectrum. We find that the Fe L lines are substantially weaker than would be expected in a collisionally excited plasma. The ratios of helium-like triplets indicate a high density. We also find evidence of an ionized absorber. We suggest the accretion flow just before it reaches the shock is the likely location for both the absorber and the low energy line emitter. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Lab Nacl Astrofis, BR-37500000 Itajuba, MG, Brazil. S African Astron Observ, ZA-7935 Cape Town, South Africa. Joint Astron Ctr, Hilo, HI 96720 USA. RP Mukai, K (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. NR 4 TC 8 Z9 8 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-091-9 J9 ASTR SOC P PY 2001 VL 251 BP 90 EP 93 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU69N UT WOS:000176731500017 ER PT B AU Elvis, M AF Elvis, M BE Inoue, H Kunieda, H TI Thermal limit spectroscopy as a goal for X-ray astronomy SO NEW CENTURY OF X-RAY ASTRONOMY SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Symposium on New Century of X-Ray Astronomy CY MAR 06-08, 2001 CL YOKOHAMA, JAPAN ID OXYGEN AB The R similar to 300-1000 grating spectra from XMM-Newton and Chandra are a radical advance, allowing spectroscopic physics techniques to be applied to X-ray astronomy, revolutionizing a wide range of research. Ten years on these spectra will be routine, and higher resolution will be needed. I propose "Thermal Limit Spectroscopy" as the next natural goal for X-ray spectroscopy. This will open up new physics: plasma physics, velocity widths, Doppler shifts, line profiles, and absorption lines in photoionized plasmas. A resolution of R = 3000-10,000 is required, and the technology is within reach. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-091-9 J9 ASTR SOC P PY 2001 VL 251 BP 180 EP 183 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU69N UT WOS:000176731500036 ER PT B AU Dalgarno, A Froelich, P Jonsell, S Saenz, A Zygelman, B AF Dalgarno, A Froelich, P Jonsell, S Saenz, A Zygelman, B BE Surko, CM Gianturco, FA TI Collisions of H and (H)over-bar SO NEW DIRECTIONS IN ANTIMATTER CHEMISTRY AND PHYSICS LA English DT Proceedings Paper CT Workshop on New Directions in Antimatter Chemistry and Physics CY OCT, 2000 CL INST THEORET ATOM & MOLEC PHYS, CAMBRIDGE, MA HO INST THEORET ATOM & MOLEC PHYS ID HYDROGEN; ANTIHYDROGEN; ANNIHILATION; ANTIPROTON AB Theoretical studies of the collisions of the atoms of hydrogen and antihydrogen at ultracold temperatures are summarised. Rearrangement may occur leading to the formation of protonium and positronium. The most probable channel yields positronium in its ground 1s state and protonium in the state with principal quantum number N = 24. The elastic cross section resulting from scattering in the Born Oppenheimer H (H) over bar potential is calculated. It is crossed by the rearrangement cross section, which is increasing inversely as the velocity, at an energy of about 2 x 10(-7) atomic units. It appears that sympathetic cooling down to perhaps 0.1K may be possible before it is overtaken by annihilation. It is pointed out that the quasi-molecule H (H) over bar has an electric dipole moment so that radiation is produced during the collision process and may serve as a diagnostic probe of the event. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dalgarno, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 14 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 0-7923-7152-6 PY 2001 BP 47 EP 52 PG 6 WC Physics, Atomic, Molecular & Chemical SC Physics GA BU78G UT WOS:000177000000004 ER PT B AU Wilkes, BJ Green, P Brissenden, R Cameron, R Dobrzycki, A Drake, J Evans, N Fruscione, A Garcia, M Ghosh, H Grimes, J Grindlay, J Hooper, E Karovska, M Kashyap, V Kim, DW Kowal, K Marshall, H Mossman, A Morris, D Nichols, J Szentgyorgyi, A Tananbaum, H van Speybroeck, L Vikhlinin, A Virani, S Zhao, P Gaetz, T Baldwin, J Kindt, A Chaffee, F Dey, A Jannuzi, B Foltz, C Mathur, S McNamara, B Newberg, H AF Wilkes, BJ Green, P Brissenden, R Cameron, R Dobrzycki, A Drake, J Evans, N Fruscione, A Garcia, M Ghosh, H Grimes, J Grindlay, J Hooper, E Karovska, M Kashyap, V Kim, DW Kowal, K Marshall, H Mossman, A Morris, D Nichols, J Szentgyorgyi, A Tananbaum, H van Speybroeck, L Vikhlinin, A Virani, S Zhao, P Gaetz, T Baldwin, J Kindt, A Chaffee, F Dey, A Jannuzi, B Foltz, C Mathur, S McNamara, B Newberg, H BE Clowes, R Adamson, A Bromage, G TI The Chandra multi-wavelength project (ChaMP): A serendipitous survey with Chandra archival data SO NEW ERA OF WIDE FIELD ASTRONOMY SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT International Conference on the New Era of Wide Field Astronomy CY AUG 21-24, 2000 CL UNIV CENT LANCASHIRE, PRESTON, ENGLAND HO UNIV CENT LANCASHIRE ID X-RAY SOURCES; CATALOG AB The launch of the Chandra X-ray Observatory in July 1999 opened a new era in X-ray astronomy. Its unprecedented < 0.5" spatial resolution and low background are providing views of the X-ray sky 10100 times fainter than previously possible. We have initiated a serendipitous survey (ChaMP) using Chandra archival data to flux limits covering the range between those reached by current satellites and those of the small area Chandra deep surveys. We estimate the survey will cover similar to 5 deg(2) per year to X-ray fluxes (2-10 keV) in the range 10(-13)-6 X 10(-16) erg cm(-2) s(-1), discovering similar to 2000 new X-ray sources, similar to 80% of which are expected to be active galactic nuclei (AGN). The ChaMP has two parts, the extragalactic survey (ChaMP) and the Galactic plane survey (ChaM-Plane). Over five years of Chandra operations, the ChaMP will provide both a major resource for Chandra observers and a key research tool for the study of the cosmic X-ray background (CXRB) and the individual source populations which comprise it. ChaMP promises profoundly new science return on a number of key questions at the current frontier of many areas of astronomy including: (1) locating and studying high redshift clusters and so constraining cosmological parameters; (2) defining the true population of AGN, including those that are absorbed, and so constraining the accretion history of the universe; (3) filling in the gap in the luminosity / redshift plane between Chandra deep and previous surveys in studying the CXRB; (4) studying coronal emission from late-type stars as their cores become fully convective; and (5) search for cataclysmic variables (CVs) and quiescent low-mass X-ray binaries (qLXMBs) to measure their luminosity functions. In this paper we summarize the status, predictions and initial results from the X-ray analysis and optical imaging. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Wilkes, BJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 11 TC 11 Z9 11 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-065-X J9 ASTR SOC P PY 2001 VL 232 BP 47 EP 52 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31N UT WOS:000175668200009 ER PT S AU Chance, K Spurr, RJD Kurosu, TP Palmer, PI Martin, RV Fiore, A Li, Q Jacob, DJ AF Chance, K Spurr, RJD Kurosu, TP Palmer, PI Martin, RV Fiore, A Li, Q Jacob, DJ BE Sasano, Y Wang, J Hayasaka, T TI Tropospheric formaldehyde measurements from the ESA GOME instrument SO OPTICAL REMOTE SENSING OF THE ATMOSPHERE AND CLOUDS II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Optical Remote Sensing of the Atmosphere and Clouds II CY OCT 09-12, 2000 CL SENDAI, JAPAN SP SPIE, Natl Space Dev Agcy Japan, Tohoku Inst Technol, NASA Langley Res Ctr, Natl Polar Orbiting Operat Environm Satellite Syst, Integrated Program Off, TRW DE remote sensing; tropospheric composition ID OZONE AB The Global Ozone Monitoring Experiment (GOME) was launched on the European Space Agency's ERS-2 satellite on April 20, 1995. GOME measures the Earth's atmosphere in the nadir geometry, using a set of spectrometers that cover the UV and visible (240-790 nm) at moderate resolution (0.2 nm in the UV, 0.4 nm in the visible), employing silicon diode array detectors. GOME takes some 30,000 spectra per day, obtaining full global coverage in three days. We directly fit GOME radiance spectra using nonlinear least-squares analysis to obtain column amounts of several trace species with significant tropospheric concentrations, including ozone (O-3), nitrogen dioxide (NO2), sulfur dioxide (SO2), and formaldehyde (HCHO). Measurements of HCHO due to biogenic activity in the troposphere are presented here. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chance, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Palmer, Paul/F-7008-2010; Martin, Randall/C-1205-2014; OI Martin, Randall/0000-0003-2632-8402; Chance, Kelly/0000-0002-7339-7577 NR 11 TC 0 Z9 0 U1 2 U2 4 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-3803-0 J9 P SOC PHOTO-OPT INS PY 2001 VL 4150 BP 1 EP 9 DI 10.1117/12.416945 PG 3 WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics GA BS18S UT WOS:000169001200001 ER PT S AU Kurosu, TP Chance, K Yokota, T Sasano, Y AF Kurosu, TP Chance, K Yokota, T Sasano, Y BE Sasano, Y Wang, J Hayasaka, T TI Polar stratospheric cloud detection from the ILAS instrument SO OPTICAL REMOTE SENSING OF THE ATMOSPHERE AND CLOUDS II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Optical Remote Sensing of the Atmosphere and Clouds II CY OCT 09-12, 2000 CL SENDAI, JAPAN SP SPIE, Natl Space Dev Agcy Japan, Tohoku Inst Technol, NASA Langley Res Ctr, Natl Polar Orbiting Operat Environm Satellite Syst, Integrated Program Off, TRW DE polar stratospheric clouds; ozone destruction; polar atmosphere ID OZONE AB We present detection methods for polar stratospheric clouds (PSCs) from the Environment Agency of Japan's Improved Limb Atmospheric Spectrometer (ILAS) instrument during the arctic winter of 1996/1997. The PSC detection methods are based on ILAS visible channel measurements in and around the oxygen A absorption band. They involve either full nonlinear or simple linear fitting of the spectra to obtain aerosol optical thickness as a function of tangent height. PSC optical thickness is determined from a subsequent linear fit to aerosol optical thickness as a function of altitude. Results for PSC optical thickness from the two methods agree reasonably well for all cases considered in this study, but only the nonlinear fitting approach allows the definitive identification of PSC events. Comparisons with operational ILAS data products show denitrification, removal of water vapor, and generally low temperatures over the vertical region of the PSC, Finally, we present a fast and simple method for the identification of possible PSC candidates from ILAS measurements. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurosu, TP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Sasano, Yasuhiro/C-2927-2009; OI Sasano, Yasuhiro/0000-0001-7470-5642; Chance, Kelly/0000-0002-7339-7577 NR 5 TC 4 Z9 4 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-3803-0 J9 P SOC PHOTO-OPT INS PY 2001 VL 4150 BP 68 EP 75 DI 10.1117/12.416946 PG 4 WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics GA BS18S UT WOS:000169001200008 ER PT J AU Ferrari, FD Ivanenko, VN AF Ferrari, FD Ivanenko, VN TI Interpreting segment homologies of the maxilliped of cyclopoid copepods by comparing stage-specific changes during development SO ORGANISMS DIVERSITY & EVOLUTION LA English DT Article DE cyclopoid; copepod; maxilliped; development; segment; homologies ID RIDGEWAYIA-KLAUSRUETZLERI; DIOITHONA-OCULATA; OITHONIDAE; CYCLOPIDAE; BELIZE; GENUS AB Development of the maxilliped of 14 species of cyclopoid copepods from 14 genera in the families Cyclopinidae, Oithonidae and Cyclopidae is described. Segment homologies are inferred from the assumption that homologous setae and arthrodial membranes are added during the same copepodid stage, and from a model of development that patterns the endopod proximally from the proximal of two endopodal segments present at the first copepodid stage, An arthrodial membrane separates the praecoxa and coxa of two Cyclopinidae and two of three Oithonidae. The praecoxa of the Cyclopinidae and the Oithonidae has two groups of setae; the praecoxa of Cyclopidae has no more than one group. The coxa of these copepods has only one group of setae; all Cyclopidae share a coxal lobe with a single seta. The endopod of these three families may include as many as five segments. In general, the distal arthrodial membrane of a segment appears to have been more labile during evolutionary history of the maxilliped than has the ventral seta which inserts on that segment. For purposes of phylogenetic analyses, uncoupling the presence of the distal arthrodial membrane of a segment from the presence of its ventral seta and analyzing each separately may provide a better way of understanding evolutionary transformations of the limb than considering the segment as the basic structural unit of the limb. C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Invertebrate Zool MRC 534, Washington, DC 20560 USA. Moscow MV Lomonosov State Univ, Fac Biol, Dept Invertebrate Zool, Moscow 119899, Russia. RP Ferrari, FD (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Invertebrate Zool MRC 534, Washington, DC 20560 USA. RI Ivanenko, Viatcheslav/B-8198-2008 OI Ivanenko, Viatcheslav/0000-0003-1255-0491 NR 26 TC 30 Z9 36 U1 0 U2 0 PU URBAN & FISCHER VERLAG PI JENA PA BRANCH OFFICE JENA, P O BOX 100537, D-07705 JENA, GERMANY SN 1439-6092 J9 ORG DIVERS EVOL JI Org. Divers. Evol. PY 2001 VL 1 IS 2 BP 113 EP 131 DI 10.1078/1439-6092-00009 PG 19 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 512NT UT WOS:000173331000004 ER PT B AU Goddard, I AF Goddard, I BE Nichols, JD TI Contraction in Fox (Meskwaki) SO PAPERS OF THE 32ND ALGONQUIAN CONFERENCE SE PAPERS OF THE ALGONQUIAN CONFERENCE LA English DT Proceedings Paper CT 32nd Algonquian Conference CY OCT 27-29, 2000 CL Montreal, CANADA ID HISTORICAL PHONOLOGY; ARAPAHO C1 Smithsonian Inst, Washington, DC 20560 USA. NR 91 TC 5 Z9 5 U1 0 U2 0 PU UNIV MANITOBA PRESS PI WINNIPEG PA 244 ENGINEERING BLDG, WINNIPEG, MANITOBA R3T 2N2, CANADA J9 PAP ALGON CONF PY 2001 VL 32 BP 164 EP 230 PG 67 WC Anthropology; Linguistics; Language & Linguistics SC Anthropology; Linguistics GA BAJ12 UT WOS:000222495900009 ER PT J AU Kink, I Laming, JM Takacs, E Porto, JV Gillaspy, JD Silver, E Schnopper, H Bandler, SR Barbera, M Brickhouse, N Murray, S Madden, N Landis, D Beeman, J Haller, EE AF Kink, I Laming, JM Takacs, E Porto, JV Gillaspy, JD Silver, E Schnopper, H Bandler, SR Barbera, M Brickhouse, N Murray, S Madden, N Landis, D Beeman, J Haller, EE TI Microcalorimeter/EBIT measurements of X-ray spectra of highly charged ions SO PHYSICA SCRIPTA LA English DT Article; Proceedings Paper CT 10th International Conference on the Physics of Highly Charged Ions (HCI 2000) CY JUL 30-AUG 03, 2000 CL CLARK KERR CAMPUS, BERKELEY, CALIFORNIA SP Amer Vacuum Soc, Lawrence Livermore Natl Lab HO CLARK KERR CAMPUS ID FE-XVII; PLASMAS AB Spectra of highly charged At, Kr, Xe and Fe ions, produced in an Electron Beam Ion Trap (EBIT), have been recorded in a broad X-ray energy band (0.2 keV to 10 keV) with a microcalorimeter detector. The first analysis of the Kr spectra has been completed and most of the spectral lines have been identified as transitions of B- to Al-like Kr. Line intensity ratios of Fe XVII have been measured and compared with theoretical models. C1 NIST, Gaithersburg, MD 20899 USA. USN, Res Lab, Washington, DC 20375 USA. MIT, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron GS Vaiana, Palermo, Italy. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. RP Kink, I (reprint author), NIST, Gaithersburg, MD 20899 USA. RI Bandler, Simon/A-6258-2010; OI Bandler, Simon/0000-0002-5112-8106; Brickhouse, Nancy/0000-0002-8704-4473; Barbera, Marco/0000-0002-3188-7420 NR 13 TC 5 Z9 6 U1 0 U2 1 PU ROYAL SWEDISH ACAD SCIENCES PI STOCKHOLM PA PUBL DEPT BOX 50005, S-104 05 STOCKHOLM, SWEDEN SN 0031-8949 J9 PHYS SCRIPTA JI Phys. Scr. PY 2001 VL T92 BP 454 EP 456 DI 10.1238/Physica.Topical.092a00454 PG 3 WC Physics, Multidisciplinary SC Physics GA 460CK UT WOS:000170288100131 ER PT J AU Kral, P Shapiro, M AF Kral, P Shapiro, M TI Nanotube electron drag in flowing liquids SO PHYSICAL REVIEW LETTERS LA English DT Article ID CARBON NANOTUBES; TRANSPORT; MICROTUBULES; SYSTEMS; TUBULES; ROPES; PUMP AB We show that electric current can be generated in metallic carbon nanotubes immersed in liquids flowing along them. Molecular layers of the liquid coat the nanotube, slip along its surface. and excite there a phonon wind, which drags free carriers in the tube. The induced electric current should allow building of nanoscale detectors or power cells. C1 Weizmann Inst Sci, Dept Chem Phys, IL-76100 Rehovot, Israel. Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Kral, P (reprint author), Weizmann Inst Sci, Dept Chem Phys, IL-76100 Rehovot, Israel. NR 42 TC 101 Z9 104 U1 6 U2 21 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JAN 1 PY 2001 VL 86 IS 1 BP 131 EP 134 DI 10.1103/PhysRevLett.86.131 PG 4 WC Physics, Multidisciplinary SC Physics GA 388QK UT WOS:000166192800033 ER PT J AU Davis, JL AF Davis, JL TI Atmospheric water-vapor signals in GPS data: synergies, correlations, signals and errors SO PHYSICS AND CHEMISTRY OF THE EARTH PART A-SOLID EARTH AND GEODESY LA English DT Article; Proceedings Paper CT 1st COST Action 716 Workshop on Towards Operational GPS Meterology CY JUL 10-12, 2000 CL OSLO, NORWAY AB I explore the-statistics of integrated water-vapor (IWV) and the ability of GPS to provide information that reflects large-scale weather systems. I demonstrate that the power spectral density (PSD) is a much more robust estimator of IWV statistics than the structure function is for long time scales. I then use the PSD to investigate the IWV statistics of simulated atmospheres. I use a random walk to approximate the Kolmogorov behavior of local atmospheric turbulence. The atmospheres I simulate contain the turbulent behavior sumperimposed on systematic changes to the IWV that might be associated with the passage of fronts. I demonstrate that the PSD associated with such frontal systems might be quite similar to those for pure turbulent behavior This result may explain why many previous studies that examined PSDs of IWV over a site concluded that the spectra was Kolmogorov. I also derive the first cross-power spectrum of IWV using GPS sites separated by similar to 500 km. At this separation, the local turbulence may be assumed to have become decorrelated. I find that even this long wavelength signal consists of components at a wide range of temporal frequencies. The IWV cross power spectrum contains significant energy even at temporal frequencies of 2-4 cycles per hour. (C) 2001 Elsevier Science Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Davis, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 13 TC 4 Z9 4 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1464-1895 J9 PHYS CHEM EARTH PT A JI Phys. Chem. Earth Pt. A-Solid Earth Geod. PY 2001 VL 26 IS 6-8 BP 513 EP 522 DI 10.1016/S1464-1895(01)00093-X PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 436DM UT WOS:000168921300027 ER PT B AU Abel, T Bryan, GL Norman, ML AF Abel, T Bryan, GL Norman, ML BE Umemura, M Susa, H TI Forming the first star in the Universe SO PHYSICS OF GALAXY FORMATION, PROCEEDINGS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT International Meeting on Physics of Galaxy Formation CY JUL 03-07, 2000 CL UNIV TSUKUBA, TSUKUBA, JAPAN HO UNIV TSUKUBA ID HYDROGEN AB We describe results from a fully self-consistent three dimensional hydrodynamical simulations of the formation of the first star in the Universe. Length scales from a few kpc (similar to 10(22) cm) to similar to 100 solar radii (similar to 10(12) cm) are followed while gravity, hydrodynamics, primordial gas chemistry and radiative processes are calculated accurately. The formation mechanism of primordial molecular clouds and a primordial protostar is discussed. As Dark Matter dominated proto-galactic halos assemble via hierarchical merging primordial gas cools through re-vibrational lines of hydrogen molecules and sinks to their centers. The high redshift analog of a molecular cloud is formed. As the densest, central parts of the cold gas become renewed gravitationally unstable a dense core of similar to 100 M-circle dot undergoes rapid contraction. At densities n > 10(9) cm(-3) a proto-stellar core 1 M-circle dot becomes fully molecular due to three-body molecular hydrogen formation and acretes from the similar to 100 M-circle dot envelope. A massive star is born. We discuss the minimum mass of the star and briefly comment on the acretion of the first protstar. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Abel, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-054-4 J9 ASTR SOC P PY 2001 VL 222 BP 129 EP 136 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS48Q UT WOS:000170040500018 ER PT J AU Alpert, YL AF Alpert, YL TI Resonance nature of the magnetosphere SO PHYSICS REPORTS-REVIEW SECTION OF PHYSICS LETTERS LA English DT Review ID GROUND-SATELLITE-OBSERVATIONS; FIELD LINE RESONANCES; GEOMAGNETIC-PULSATIONS; ELECTROMAGNETIC-WAVES; COMPLEX SHAPE; LOW FREQUENCY; GENERATION; PC1; MICROPULSATIONS; WHISTLERS AB A new approach toward an understanding of the nature of low frequency e.m. waves (f <<, 1-250 mHz. It overlaps the frequency band of so-called Pc2-Pc5 micropulsations. Repetitive and non-repetitive single Pc1 micropulsations at f approximate to 0.4-2.2 Hz are also briefly discussed here. Under different conditions they should be created, respectively, by interaction of a non-linear and/or only linear gyro-resonance instability mechanism. The oscillations considered exist at any time both in quiet (QC) and disturbed (DC) conditions. Their spectra possess a line structure. The background is composed of resonance oscillations, and weaker oscillations caused by noise. The resonance oscillations may occur in the entire magnetosphere or in its parts. In the frequency range examined 12, 20-25, and more resonance frequencies f(s,res) were accordingly found in the spectra of the NP and SP observation points (L similar or equal to 13) and in the Tuckerton and Point Arena (L similar or equal to 2.6) data. The higher-order resonance maxima are overlapped by the noise oscillations. All these oscillations can be set swinging, producing strong non-repetitive wave packets with durations tau (0) approximate to 20-300 s and longer. The conditions for producing the swinging background can be impulse/shock excitations of the magnetospheric plasma, a gyro-resonance instability, etc. Thus, the well-known multiple manifestations of hydromagnetic wave packets observed in our research in the magnetosphere at f < 0.25 Hz are considered to be the result of a single physical phenomenon: the fundamental resonance e.m. oscillatory nature of the background magnetospheric plasma environment. It is shown that the observed waves and the spectral resonance oscillations are temporally modulated by extra-low-frequency oscillations f(mod) 1.8-2.0 mHz < and << f(s,res). We believe that these oscillations are of Solar origin and were transferred to the Earth by the Solar wind. By analyzing calculated Fourier spectra of different kinds of wave packets - signals F(t) - we have found that any continuum of spectral maximal f(s,max) of these F(t) is characterized by a quasi-constant quantity - the spectral shape characteristic. It estimates the general image of the envelope of the signals and their duration. (C) 2001 Elsevier Science B.V. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Alpert, YL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM alpert@cfa.harvard.edu NR 68 TC 2 Z9 2 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-1573 J9 PHYS REP JI Phys. Rep.-Rev. Sec. Phys. Lett. PD JAN PY 2001 VL 339 IS 5-6 BP 324 EP 444 PG 121 WC Physics, Multidisciplinary SC Physics GA 389FM UT WOS:000166228000002 ER PT J AU Hood, WR Kunz, TH Oftedal, OT Iverson, SJ LeBlanc, D Seyjagat, J AF Hood, WR Kunz, TH Oftedal, OT Iverson, SJ LeBlanc, D Seyjagat, J TI Interspecific and intraspecific variation in proximate, mineral, and fatty acid composition of milk in old world fruit bats (Chiroptera : Pteropodidae) SO PHYSIOLOGICAL AND BIOCHEMICAL ZOOLOGY LA English DT Article ID LACTATION; NITROGEN; WEIGHTS; ENERGY; BODY AB We examine the effect of body mass on milk composition among Old World fruit bats, including Pteropus pumilus (0.175 kg), Pteropus rodricensus (0.265 kg), Pteropus hypomelanus (0.571 kg), and Pteropus vampyrus (1.133 kg). We describe intra- and interspecific differences in the proximate composition of milk among these four species and the minerals and fatty acids in the milk of the latter two species. There were no differences between species in the concentrations of dry matter, fat, or lactose in milk. However, there were significant, although small, differences in the protein content of milk among species, with protein being significantly greater in P. rodricensus than in P. pumilus and P. hypomelanus and protein being significantly less in P. hypomelanus than in P. rodricensus and P. vampyrus. There were no differences in mineral content between P. hypomelanus and P. vampyrus in milk minerals, but minor differences were evident in fatty acids 12:0, 14:0, 18:0, 18:1n11, and 18:2n6. Our findings suggest that milk composition is relatively constant across lactation for most proximate, mineral, and fatty acid components. We found a significant increase in dry matter and energy across lactation in the concentration of dry matter and energy in P. pumilus and fat in P. hypomelanus. In P. hypomelanus, we found a significant increase in the concentration of fatty acids 10:0 and 20:1n9 and a significant decrease in Iso15 and 20:1n7. No other differences associated with day of lactation were found. These findings suggest that milk composition is generally similar within the genus Pteropus, despite a 6.5-fold difference in body mass between species that we evaluated. C1 Boston Univ, Dept Biol, Boston, MA 02215 USA. Fordham Univ, Louis Calder Ctr, Armonk, NY 10504 USA. Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. Dalhousie Univ, Dept Biol, Halifax, NS B3H 4J1, Canada. Lubee Fdn Inc, Gainesville, FL 32609 USA. RP Hood, WR (reprint author), Boston Univ, Dept Biol, 5 Cummington St, Boston, MA 02215 USA. EM hood@fordham.edu NR 69 TC 10 Z9 10 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1522-2152 EI 1537-5293 J9 PHYSIOL BIOCHEM ZOOL JI Physiol. Biochem. Zool. PD JAN-FEB PY 2001 VL 74 IS 1 BP 134 EP 146 DI 10.1086/319305 PG 13 WC Physiology; Zoology SC Physiology; Zoology GA 408VB UT WOS:000167347200014 PM 11226022 ER PT J AU Schmidt, G Zotz, G AF Schmidt, G Zotz, G TI Ecophysiological consequences of differences in plant size: in situ carbon gain and water relations of the epiphytic bromeliad, Vriesea sanguinolenta SO PLANT CELL AND ENVIRONMENT LA English DT Article DE Vriesea sanguinolenta; ecophysiology; epiphytes; heteroblasty; photosynthesis; plant size; stomatal behaviour; water relations ID LEAF GAS-EXCHANGE; PHOTOSYNTHETIC CAPACITY; MIDDAY DEPRESSION; EFFICIENCY; LEAVES; PERMEABILITY; DROUGHT; MODEL AB This held study with the C-3 bromeliad Vriesea sanguinolenta (Cogn, & Marchal 1874) was initiated to explore the importance of size-related ecophysiological changes in vascular epiphytes in a natural tropical setting, In this species, a step change from atmospheric to tank-forming life form occurs during early ontogeny, followed by a continuous size increase of individuals with water-impounding tanks. Although our study focused on the wafer-impounding phase, this growth pattern also allowed us to compare ecophysiological consequences of a step change in life form with those associated with size increments among plants of identical life form. The shift in life form was accompanied by relatively minor changes, for example in leaf morphology (decrease in leaf thickness and trichome density) and leaf physiology (decrease in photosynthetic capacity), while there were more substantial changes during the tank-forming phase. A major trend was a decreasing dependence of larger plants on internally stored water due to a more efficient tank. We suggest that the resulting, more reliable wafer supply in larger plants may be the proximate cause for the observed size-related differences in leaf anatomy (relative reduction of wafer storage tissue, and relative and absolute increase in chlorenchyma thickness), leaf morphology (increase in stomatal density, decrease in trichome density), and leaf physiology (increase in net rates of CO2 uptake, more conservative stomatal behaviour, higher residual transpiration). The results are compared with previous studies on heteroblasty in bromeliads, but are also discussed in the context of a gradual shift from a drought-tolerance to a drought-avoidance strategy. C1 Univ Wurzburg, Lehrstuhl Bot 2, D-97082 Wurzburg, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Schmidt, G (reprint author), Univ Wurzburg, Lehrstuhl Bot 2, D-97082 Wurzburg, Germany. NR 36 TC 42 Z9 43 U1 0 U2 28 PU BLACKWELL SCIENCE LTD PI OXFORD PA P O BOX 88, OSNEY MEAD, OXFORD OX2 0NE, OXON, ENGLAND SN 0140-7791 J9 PLANT CELL ENVIRON JI Plant Cell Environ. PD JAN PY 2001 VL 24 IS 1 BP 101 EP 111 DI 10.1046/j.1365-3040.2001.00658.x PG 11 WC Plant Sciences SC Plant Sciences GA 399CU UT WOS:000166794200009 ER PT S AU Stephens, CE AF Stephens, CE GP IEEE IEEE TI Engineering time: Inventing the quartz wristwatch SO PROCEEDINGS OF THE 2001 IEEE INTERNATIONAL FREQUENCY CONTROL SYMPOSIUM & PDA EXHIBITION SE PROCEEDINGS OF THE IEEE INTERNATIONAL FREQUENCY CONTROL SYMPOSIUM LA English DT Proceedings Paper CT IEEE International Frequency Control Symposium and PDA Exhibition CY JUN 06-08, 2001 CL SEATTLE, WA SP IEEE Ultrason Ferroelect & Frequency Control Soc, EIA Electr Components Assemblies & Mat Assoc C1 Smithsonian Inst, Natl Mus Amer Hist, Washington, DC USA. RP Stephens, CE (reprint author), Smithsonian Inst, Natl Mus Amer Hist, Washington, DC USA. NR 6 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1075-6787 BN 0-7803-7028-7 J9 P IEEE INT FREQ CONT PY 2001 BP 2 EP 3 DI 10.1109/FREQ.2001.956151 PG 2 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Physics, Condensed Matter SC Engineering; Instruments & Instrumentation; Physics GA BU18C UT WOS:000175262100001 ER PT B AU Allen, ME AF Allen, ME BE Edwards, MS Lisi, KJ Schlegel, ML Bray, RE TI So, you want to be a zoo animal nutritionist! SO PROCEEDINGS OF THE AZA NUTRITION ADVISORY GROUP FOURTH CONFERENCE ON ZOO AND WILDLIFE NUTRITION LA English DT Proceedings Paper CT 4th AZA Nutrition-Advisory-Group Conference on Zoo and Wildlife Nutrition CY SEP 19-23, 2001 CL Orlando, FL SP Disneys Anim Kingdom, Amer Zoo & Aquarium Assoc, Nutrit Advisory Grp DE comparative nutrition; education; practical experience; animal diets; nutrient requirements C1 Smithsonian Inst, Dept Conservat Biol, Washington, DC 20560 USA. RP Allen, ME (reprint author), Smithsonian Inst, Dept Conservat Biol, Natl Zool Pk, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ZOO & AQUARIUM ASSOC (AZA) PI SILVER SPRING PA 8403 COLESVILLE RD, SUITE 710, SILVER SPRING, MD 20910 USA PY 2001 BP 1 EP 3 PG 3 WC Agriculture, Dairy & Animal Science; Nutrition & Dietetics; Zoology SC Agriculture; Nutrition & Dietetics; Zoology GA BY87F UT WOS:000189483500001 ER PT J AU Huang, YM AF Huang, YM TI A pictorial key for the identification of the subfamilies of Culicidae, genera of Culicinae, and subgenera of Aedes mosquitoes of the Afrotropical Region (Diptera : Culicidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE pictorial key; identification; subfamilies; genera; mosquitoes; subgenera of Aedes; Afrotropical Region AB A pictorial key is presented as a field aid for the identification of adult mosquitoes of 3 subfamilies of Culicidae, 15 genera of Culicinae, and II subgenera of Aedes occurring in the Afrotropical Region. Scanning electron micrographs demonstrate the taxonomic characters used in the key. C1 Smithsonian Inst, Dept Entomol, MRC 534, Washington, DC 20560 USA. RP Huang, YM (reprint author), Smithsonian Inst, Dept Entomol, MRC 534, NHB 169, Washington, DC 20560 USA. NR 11 TC 23 Z9 24 U1 0 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 2001 VL 103 IS 1 BP 1 EP 53 PG 53 WC Entomology SC Entomology GA 395KA UT WOS:000166578500001 ER PT J AU Gagne, RJ Oda, RAM Monteiro, RF AF Gagne, RJ Oda, RAM Monteiro, RF TI The gall midges (Diptera : Cecidomyiidae) of Mikania glomerata (Asteraceae) in southeastern Brazil SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE neotropical; gall midges; gall makers; Asteraceae AB A survey of Mikania glomerata Sprengel (Eupatorieae: Asteraceae) in southeastern Brazil resulted in the discovery of eight kinds of galls made by eight species of gall midges. All of the galls and their gall makers are described. Seven of the gall makers are new to science and two new genera, Liodiplosis Gagne and Mikaniadiplosis Gagne, are described to contain four of the seven new species. The eight gall-making species are: Alycaulus globulus Gagne, Asphondylia glomeratae Gagne, Asphondylia moehni Skuhrava, Liodiplosis cylindrica Gagne, Liodiplosis conica Gagne, Liodiplosis spherica Gagne, Mikaniadiplosis annulipes Gagne, and Perasphondylia mikaniae Gagne. In addition, another gall midge new to science, Contarinia ubiquita Gagne, is described that lives gregariously in the galls of five of the eight kinds of galls described. C1 ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20560 USA. UFRJ, Lab Ecol Insetos, Dept Ecol, IB, BR-21941590 Rio De Janeiro, Brazil. RP Gagne, RJ (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20560 USA. RI Monteiro, Ricardo/J-3974-2012 NR 15 TC 2 Z9 5 U1 1 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JAN PY 2001 VL 103 IS 1 BP 110 EP 134 PG 25 WC Entomology SC Entomology GA 395KA UT WOS:000166578500009 ER PT S AU Korzennik, SG AF Korzennik, SG BE Wilson, A TI On the diagnostic potential of time-distance helioseismology SO PROCEEDINGS OF THE SOHO 10/GONG 2000 WORKSHOP ON HELIO- AND ASTEROSEISMOLOGY AT THE DAWN OF THE MILLENNIUM SE ESA Special Publications LA English DT Proceedings Paper CT SOHO 10/GONG 2000 Workshop on Helio- and Asteroseismology at the Dawn of the Millennium CY OCT 02-06, 2000 CL INST ASTROFIS CANARIAS, SANTA CRUZ TENERI, SPAIN SP Spanish Minist Sci & Technol, European Space Agcy, Global Oscillat Network Grp HO INST ASTROFIS CANARIAS DE sun : oscillations; time-distance AB Time-distance analysis has proven to be a powerful and intuitively self evident approach for local helioseismology. By directly measuring propagation times of wave packets between selected locations at the surface, and their variations over a specific area of the sun, a directed diagnostic of the physical properties of that region can be achieved. The empirical approach taken by most investigators appears to be robust and has produced enticing results. But surprisingly, the theoretical framework for time-distance seismology remains sketchy. At the same time, rigorous inversion methodologies need to be further developed and validated; and, as in any inverse problem, the topology of the underlying anihilator must be well understood to adequately interpret the inferred properties. Using simulated observables and focusing on the inference of the velocity flow, I illustrate the diagnostic potential of time-distance inversion and its limitation with simple and realistic simulations. I also present inversions based on actual observations obtained with the MDI instrument on board SOHO. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Korzennik, SG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM skorzennik@cfa.harvard.edu NR 15 TC 3 Z9 3 U1 0 U2 0 PU ESA PUBLICATIONS DIVISION C/O ESTEC PI 2200 AG NOORDWIJK PA PO BOX 299, 2200 AG NOORDWIJK, NETHERLANDS SN 0379-6566 BN 92-9092-697-X J9 ESA SPEC PUBL PY 2001 VL 464 BP 149 EP 156 PG 8 WC Astronomy & Astrophysics; Physics, Applied SC Astronomy & Astrophysics; Physics GA BS21T UT WOS:000169104500027 ER PT S AU Weekes, TC AF Weekes, TC BE Saltzberg, D Gorham, P TI Radio pulses from cosmic ray air showers SO RADIO DETECTION OF HIGH ENERGY PARTICLES SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 1st International Workshop on Radio Detection of High Energy Particles (RADHEP 2000) CY NOV 16-18, 2000 CL LOS ANGELES, CA SP Univ Calif Los Angeles AB The first experiment in which radio emission was detected from high energy particles is described. An array of dipoles was operated by a team of British and Irish physicists in 1964-5 at the Jodrell Bank Radio Observatory in conjunction with a simple air shower trigger. The array operated at 44 MHz with 2.75 MHz bandwidth. Out of 4.500 triggers a clear bandwidth-limited radio pulse was seen in 11 events. This corresponded to a cosmic ray trigger threshold of 5x10(16) eV and was of intensity close to that predicted. The early experiments which followed this discovery and their interpretation is described. C1 Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. RP Weekes, TC (reprint author), Harvard Smithsonian Ctr Astrophys, Whipple Observ, POB 97, Amado, AZ 85645 USA. NR 22 TC 8 Z9 8 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0018-0 J9 AIP CONF PROC PY 2001 VL 579 BP 3 EP 13 PG 11 WC Physics, Particles & Fields SC Physics GA BS97M UT WOS:000171562900001 ER PT S AU Cranmer, SR AF Cranmer, SR BE Mau, TK DeGrassie, J TI Ion cyclotron damping in the solar corona and solar wind SO RADIO FREQUENCY POWER IN PLASMAS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 14th Topical Conference on Radio Frequency Power in Plasmas CY MAY 07-09, 2001 CL OXNARD, CA SP Gen Atom, Univ Calif San Diego, Amer Inst Phys ID MAGNETOHYDRODYNAMIC TURBULENCE; TRANSITION REGION; MAGNETIC-FIELD; FREQUENCY WAVES; ALFVEN WAVES; ACCELERATION; HOLES; MODEL; SUN; CONSTRAINTS AB The solar corona is the hot, ionized outer atmosphere of the Sun. Coronal plasma expands into interplanetary space as a supersonic bulk outflow known as the solar wind. This tenuous and unbounded medium is a unique laboratory for the study of kinetic theory in a nearly collisionless plasma, as well as magnetohydrodynamic waves, shocks, and jets. Particle velocity distributions in the solar wind have been probed directly by spacecraft (outside the orbit of Mercury), and indirectly by ultraviolet spectroscopy (close to the Sun). Fluctuations in the plasma properties and in electromagnetic fields have been measured on time scales ranging from seconds to years. Despite more than a half-century of study, though, the basic physical processes responsible for heating the million-degree corona and accelerating the solar wind past the Sun's escape velocity are still not known with certainty. Understanding the basic physics of the solar wind is necessary to predict the Sun's impact on the Earth's climate and local space environment. This presentation will review the kinetic origins of several physical processes that are currently believed to be important in depositing energy and momentum in coronal particle velocity distributions. Because ions in the solar wind are heated and accelerated more than would be expected in either thermodynamic equilibrium or via a mass-proportional process, an ion cyclotron resonance has been suggested as a likely mechanism. Other evidence for gyroresonant wave dissipation in the corona will be presented, and possible generation mechanisms for the (as yet unobserved) high-frequency cyclotron waves will be reviewed. The mean state of the coronal and heliospheric plasma is intimately coupled with kinetic fluctuations about that mean, and theories of turbulence, wave dissipation, and instabilities must continue to be developed along with steady state descriptions of the solar wind. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 44 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0038-5 J9 AIP CONF PROC PY 2001 VL 595 BP 25 EP 32 PG 8 WC Physics, Fluids & Plasmas SC Physics GA BT43V UT WOS:000173023300003 ER PT S AU Parenti, S Bromage, BJI Poletto, G Noci, G Raymond, JC Bromage, GE AF Parenti, S Bromage, BJI Poletto, G Noci, G Raymond, JC Bromage, GE BE Brekke, P Fleck, B Gurman, JB TI Properties of different coronal streamers SO RECENT INSIGHTS INTO THE PHYSICS OF THE SUN AND HELIOSPHERE: HIGHLIGHTS FROM SOHO AND OTHER SPACE MISSIONS SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 24th General Assembly of the International-Astronomical-Union CY AUG 07-18, 2000 CL MANCHESTER, ENGLAND SP Int Astron Union AB In this paper a summary of results from coordinated observations of streamers acquired by the SOHO Coronal Diagnostic Spectrometer (CDS) and UltraViolet Coronograph Spectrometer (UVCS) experiments is presented (Parenti et al. 2000). Data from different altitudes within the solar corona were taken, with the purpose of determining their physical parameters - densities, electron temperatures and element abundances - and their changes over the altitude range between 1.02 and 1.6 R-circle dot. Further UVCS streamer data, taken about two months later are used to compare with the behaviour seen in two different streamers. The streamers resulted to have a different behaviour in temperature and density. The low corona, covered by CDS data, shows little evidence of abundance variation with respect to photospheric values, while, at UVCS altitudes, a depletion of all element abundances is clearly evident. C1 Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Univ Florence, I-50125 Florence, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Parenti, S (reprint author), Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA SN 0074-1809 BN 1-58381-069-2 J9 IAU SYMP PY 2001 IS 203 BP 413 EP 415 PG 3 WC Astronomy & Astrophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Meteorology & Atmospheric Sciences GA BU43X UT WOS:000175997400096 ER PT J AU Roth, TL O'Brien, JK McRae, MA Bellem, AC Romo, SJ Kroll, JL Brown, JL AF Roth, TL O'Brien, JK McRae, MA Bellem, AC Romo, SJ Kroll, JL Brown, JL TI Ultrasound and endocrine evaluation of the ovarian cycle and early pregnancy in the Sumatran rhinoceros, Dicerorhinus sumatrensis SO REPRODUCTION LA English DT Article ID CAMEL CAMELUS-DROMEDARIUS; CERATOTHERIUM-SIMUM SIMUM; ENZYME-IMMUNOASSAY; DICEROS-BICORNIS; ESTROUS-CYCLE; OVULATION; PROGESTERONE; PREGNANEDIOL-3-GLUCURONIDE; FOLLICULOGENESIS; METABOLISM AB Longitudinal ultrasound and endocrine evaluations were conducted in two adult female Sumatran rhinoceroses (Dicerorhinus sumatrensis) over a period of 12-22 months to learn move about their reproductive physiology. Rectal ultrasonography was conducted to monitor ovarian activity. Blood samples were collected and analysed for progesterone and LH, and faecal samples were analysed for progestin metabolites. One female showed cyclic ovarian activity during the study period, whereas the other female showed no evidence of ovarian activity. The cyclic Sumatran rhinoceros appeared to be an induced ovulator, the first of its kind reported within the Perrisodactyla. Ultrasound examinations of the ovaries revealed the formation of anovulatory haemorrhagic follicles when the animal was not mated. These follicles appeared to undergo varied degrees of luteinization that resulted in irregular faecal progestin profiles. When allowed to mate, the female showed a 21 day reproductive cycle that was reflected in both faecal progestin and serum progesterone profiles. The concentration of serum LH was baseline before mating, increased approximately 30-fold within 1-2 h of intromission and returned to baseline within 22 h. Ovulation occurred within 46 h of copulation. The female conceived three times during the study, pregnancy was detected using ultrasonography 14-16 days after mating, and the concentration of both serum progesterone and faecal progestins remained high. Early embryogenesis appeared to be similar to that in horses. However, each pregnancy terminated unexpectedly within the first 3 months of gestation. This study demonstrates the important role that basic research and reproductive technology can play in developing a natural breeding programme for an endangered animal in captivity. C1 Cincinnati Zoo & Bot Garden, Ctr Res Endangered Wildlife, Cincinnati, OH 45220 USA. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Roth, TL (reprint author), Cincinnati Zoo & Bot Garden, Ctr Res Endangered Wildlife, Cincinnati, OH 45220 USA. NR 35 TC 35 Z9 39 U1 0 U2 7 PU JOURNALS OF REPRODUCTION FERTILITY LTD PI CAMBRIDGE PA 22 NEWMARKET RD, CAMBRIDGE CB5 8DT, ENGLAND SN 1470-1626 J9 REPRODUCTION JI Reproduction PD JAN PY 2001 VL 121 IS 1 BP 139 EP 149 PG 11 WC Developmental Biology; Reproductive Biology SC Developmental Biology; Reproductive Biology GA 426BF UT WOS:000168328900014 PM 11226037 ER PT B AU Arce, HG Goodman, AA AF Arce, HG Goodman, AA BE Wootten, A TI New components of outflows from young stars revealed through high-resolution SO SCIENCE WITH THE ATACAMA LARGE MILLIMETER ARRAY SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Science with the Atacama Large Millimeter Array CY OCT 06-08, 1999 CL CARNEGIE INST WASHINGTON, WASHINGTON, D.C. SP Assoc Univ Inc, Natl Radio Astron Observ HO CARNEGIE INST WASHINGTON ID CO; FLOWS; JETS AB New millimeter observations with simultaneously high spatial and velocity resolution reveal new components of molecular outflows from young stellar objects. As an example, we show how localized high-velocity components in the PV Cephei outflow, discovered with the IRAM 30-m telescope, were detected not only due to high velocity resolution spectra, but also due to the IRAM 30m's high spatial resolution. We argue that "outflow" material may not be just that associated with high-velocity, low-column density line wings or bumps in CO spectra, but may instead account for a substantial fraction of the total column density along many lines of sight. If this conjecture is true, models of the clump mass function in molecular clouds may need reinterpretation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Arce, HG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-072-2 J9 ASTR SOC P PY 2001 VL 235 BP 99 EP 102 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31Q UT WOS:000175670700009 ER PT B AU Di Francesco, J Myers, PC Wilner, DJ AF Di Francesco, J Myers, PC Wilner, DJ BE Wootten, A TI Millimeter interferometer mosaics of clusters in formation SO SCIENCE WITH THE ATACAMA LARGE MILLIMETER ARRAY SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Science with the Atacama Large Millimeter Array CY OCT 06-08, 1999 CL CARNEGIE INST WASHINGTON, WASHINGTON, D.C. SP Assoc Univ Inc, Natl Radio Astron Observ HO CARNEGIE INST WASHINGTON AB Stars form typically in clusters, in short time intervals (< 1 Myr) and in small regions of turbulent dense gas (< 0.5 pc across). Millimeter interferometers can now provide wide-field, high-resolution observations of protoclusters, where objects are typically too closely spaced and too embedded to observe by any other means. Following Testi & Sargent (1998), who mosaicked the Serpens NW+SE protocluster with the OVRO Millimeter Array, we have observed mosaics of other regions with high surface densities of protostellar objects, including the OMC-2/3 region in Orion, the L1551 region in Taurus, the NGC 1333 IRAS 4 region in Perseus, and the rho Oph A filament of Ophiuchus. Mosaics of lambda = 3.2 mm continuum were made alongside mosaics of the N2H+ (1-0) line, a tracer of dense gas (e.g., n(cr) approximate to 2 x 10(5) cm(-3)) that avoids confusion from outflow motions. These mosaics will provide key constraints to cluster formation models by revealing the relative spacings, masses, and velocities of the protostellar objects in very young clusters. In addition, they demonstrate a compelling future programme for ALMA. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Di Francesco, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-42, Cambridge, MA 02138 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-072-2 J9 ASTR SOC P PY 2001 VL 235 BP 121 EP 124 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31Q UT WOS:000175670700014 ER PT B AU Wilner, DJ DePree, CG Goss, WM Welch, WJ McGrath, E AF Wilner, DJ DePree, CG Goss, WM Welch, WJ McGrath, E BE Wootten, A TI Subarcsecond observations of high mass star formation in the W49N region SO SCIENCE WITH THE ATACAMA LARGE MILLIMETER ARRAY SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Science with the Atacama Large Millimeter Array CY OCT 06-08, 1999 CL CARNEGIE INST WASHINGTON, WASHINGTON, D.C. SP Assoc Univ Inc, Natl Radio Astron Observ HO CARNEGIE INST WASHINGTON AB We present multi-frequency subarcsecond images of the high mass star forming region W49N. The images, with resolution from 0".045 (VLA at 7 mm) to 0".35 (BIMA at 3.3 mm), obtain high dynamic range in an environment of complex emission, a hint of the capabilities to come with ALMA. The W49N core contains more than a dozen ultracompact HII regions arranged in a 2 pc diameter ring. The new millimeter images resolve the individual ultracompact HII regions at the 500 AU scale and show that many have shell or ring morphologies. The sources with rising radio spectral indices to shorter wavelengths also have the broadest H66alpha recombination lines (DeltaV(fwhm) > 45 km s(-1)), phenomena likely explained by the presence of powerful ionized winds. No sources show a break in their radio spectrum at 3.3 mm corresponding to dust emission. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wilner, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-072-2 J9 ASTR SOC P PY 2001 VL 235 BP 175 EP 178 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31Q UT WOS:000175670700026 ER PT B AU Zhang, Q Hunter, TR Sridharan, TK Kawamura, JH AF Zhang, Q Hunter, TR Sridharan, TK Kawamura, JH BE Wootten, A TI A Disk/Outflow system around the high-mass protostar IRAS 20126+4104 SO SCIENCE WITH THE ATACAMA LARGE MILLIMETER ARRAY SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Science with the Atacama Large Millimeter Array CY OCT 06-08, 1999 CL CARNEGIE INST WASHINGTON, WASHINGTON, D.C. SP Assoc Univ Inc, Natl Radio Astron Observ HO CARNEGIE INST WASHINGTON ID (PROTO)STAR IRAS-20126+4104; OUTFLOW AB We present images of a disk/outflow system around a high-mass protostar IRAS 20126+4104. In the NH3 (1,1) and (2,2) lines, we have resolved a flattened disk-like structure (6" x 3" or 10000 x 5000 AU). The disk rotates faster toward the center, consistent with the Keplerian motion. In the direction roughly perpendicular to the disk, there exists a warm bipolar CO (7-6) outflow and the shock excited NH3 (3,3). The CO (7-6) outflow is much more compact and appears in a different orientation from the arcminute-scale north-south flow seen in the CO (2-1). Since most of the high-mass stars are formed in cluster environment and are located at kiloparsec distances, sensitive and high resolution observations of high density and highly excited molecular transitions are crucial to pinpoint the massive objects. Designed to have those capabilities, ALMA will make a significant contribution to the understanding of the protostellar environment of high-mass stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhang, Q (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-072-2 J9 ASTR SOC P PY 2001 VL 235 BP 191 EP 194 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31Q UT WOS:000175670700030 ER PT B AU Calvet, N D'Alessio, P AF Calvet, N D'Alessio, P BE Wootten, A TI YSO disk structure and planetary signatures SO SCIENCE WITH THE ATACAMA LARGE MILLIMETER ARRAY SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Science with the Atacama Large Millimeter Array CY OCT 06-08, 1999 CL CARNEGIE INST WASHINGTON, WASHINGTON, D.C. SP Assoc Univ Inc, Natl Radio Astron Observ HO CARNEGIE INST WASHINGTON ID T-TAURI-STARS; IRAS OBSERVATIONS; ACCRETION; EVOLUTION; NEBULA; DUST AB Detailed radial/vertical structure modeling of observations of disks around Young Stellar Objects (YSOs) can provide information on the physical conditions and on the characteristics of the gas and dust in their interiors. We describe recent results of self-consistent modeling of spectral energy distributions, optical and infrared images, and millimeter fluxes of YSOs. We discuss observations and interpretations of the initial stages of planet formation, including indications of dust growth and settling in disks around young stars. We also discuss how the unprecedented resolution and sensitivity of ALMA may help us study the interior of the innermost disks, a region unaccessible with present day instrumentation, and witness the very first stages of planet formation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Calvet, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. NR 34 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-072-2 J9 ASTR SOC P PY 2001 VL 235 BP 205 EP 214 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31Q UT WOS:000175670700032 ER PT B AU Gurwell, MA Muhleman, DO Butler, BJ AF Gurwell, MA Muhleman, DO Butler, BJ BE Wootten, A TI Planetary atmospheric science with ALMA SO SCIENCE WITH THE ATACAMA LARGE MILLIMETER ARRAY SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Science with the Atacama Large Millimeter Array CY OCT 06-08, 1999 CL CARNEGIE INST WASHINGTON, WASHINGTON, D.C. SP Assoc Univ Inc, Natl Radio Astron Observ HO CARNEGIE INST WASHINGTON AB The Atacama Large Millimeter Array will be one of the premier earth-based observatories for studying the atmospheres of nearly all solar system objects, including "almost airless" bodies such as Io and comets at moderate heliocentric distances as well as the more extensive atmospheres of both terrestrial and giant planets. Analysis of spatially resolved observations of pressure-broadened lines allows for three-dimensional mapping of temperature and species abundances, information that is often unattainable by other means. In addition, mapping the Doppler shift of line cores is a direct measure of the global atmospheric circulation. The high sensitivity and resolution provided by ALMA will allow precise atmospheric observations of the atmospheres of even small bodies such as Titan, Triton, and the Pluto-Charon system. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gurwell, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 4 TC 0 Z9 0 U1 0 U2 2 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-072-2 J9 ASTR SOC P PY 2001 VL 235 BP 229 EP 232 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31Q UT WOS:000175670700035 ER PT B AU Wiedner, MC Hills, RE AF Wiedner, MC Hills, RE BE Wootten, A TI Getting a clear view through the atmosphere radiometric phase correction at 183 GHz SO SCIENCE WITH THE ATACAMA LARGE MILLIMETER ARRAY SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Science with the Atacama Large Millimeter Array CY OCT 06-08, 1999 CL CARNEGIE INST WASHINGTON, WASHINGTON, D.C. SP Assoc Univ Inc, Natl Radio Astron Observ HO CARNEGIE INST WASHINGTON AB Just as ground based optical astronomy is limited by "seeing" caused by temperature differences in air, the resolution in (sub) millimeter interferometry is severely limited by fluctuating amounts of water vapor in the atmosphere. In optical astronomy the wavefront can be mostly restored using adaptive optics, here we describe a successful correction method using two 183 GHz heterodyne radiometers at the CSO-JCMT interferometer. Further development of such techniques will enable future telescopes, such as ALMA, to reach their full capability, providing resolution of order 0.01". C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wiedner, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 78, Cambridge, MA 02138 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-072-2 J9 ASTR SOC P PY 2001 VL 235 BP 253 EP 256 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31Q UT WOS:000175670700041 ER PT B AU Holec, P Emry, RJ AF Holec, P Emry, RJ BE Novotny, J TI Cenozoic primates of Slovakia SO SCRIPTA FACULTATIS SCIENTIARUM NATURALIUM UNIVERSITATIS MASARYKIANAE BRUNENSIS - GEOLOGY, VOL 30/2000 LA English DT Proceedings Paper CT 13th Conference on Upper Tertiary CY APR 19-20, 2001 CL BRNO, CZECH REPUBLIC SP Masaryk Univ Brno, Dept Geol & Palaeontol, Czech Geol Survey, Brno Branch DE primates; Cenozoic; Slovak Republic ID TURKEY AB The article gives summary of the findings of the Primates from Area of Slovak Republic without of the Familie Hominidae. C1 Comenius Univ, Fac Sci, Dept Geol & Paleontol, Bratislava 84215, Slovakia. Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Holec, P (reprint author), Comenius Univ, Fac Sci, Dept Geol & Paleontol, Bratislava 84215, Slovakia. NR 21 TC 0 Z9 0 U1 0 U2 0 PU MASARYKOVA UNIVERZITA PI BRNO PA ZENOTINOVO NAM 9, BRNO 60177, CZECH REPUBLIC BN 80-210-2678-2 PY 2001 BP 109 EP 113 PG 5 WC Geology SC Geology GA BV03M UT WOS:000177660900013 ER PT S AU Ko, YK Zurbuchen, T Strachan, L Riley, P Raymond, JC AF Ko, YK Zurbuchen, T Strachan, L Riley, P Raymond, JC BE WimmerSchweingruber, RF TI A solar wind coronal origin study from SOHO/UVCS and ACE/SWICS joint analysis SO SOLAR AND GALACTIC COMPOSITION SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Joint SOHO/ACE Workshop on Solar and Galactic Composition CY MAR 06-09, 2001 CL BERN, SWITZERLAND SP European Space Agcy, Schweizer Natl Fonds Forder Wissensch, Oerlikon Contraves Space SA, Univ Bern, Physikal Inst ID SPECTROMETER AB The solar wind ionic charge composition is a powerful tool to distinguish between the slow wind and the coronal-hole associated fast wind. The solar wind heavy ions axe believed to be 'frozen-in' within 5 solar radii of the Sun which falls right in the range of SOHO/UVCS coronal observations. We present a joint analysis from SOHO/UVCS and ACE/SWICS which attempts to establish observational evidence of the coronal origin of the solar wind. To connect the solar wind with its coronal origin, we adopt a 3-D MHD model as a guide to link the solar wind at 1 AU to structures in the inner corona. We relate in-situ measured properties of the solar wind (elemental abundances and charge state distributions) with remotely sensed signatures in the corona, namely outflow velocity, electron temperature and elemental abundance. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ko, YK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 15 TC 3 Z9 3 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0042-3 J9 AIP CONF PROC PY 2001 VL 598 BP 133 EP 138 PG 6 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA BT59T UT WOS:000173445900020 ER PT J AU Habbal, SR Woo, R Vial, JC AF Habbal, SR Woo, R Vial, JC TI UVCS observations of velocity shear at streamer boundaries in the corona SO SPACE SCIENCE REVIEWS LA English DT Review ID SPECTROMETER; SOLAR AB Measurements of the intensities of the O VI 1032 and 1037 Angstrom spectral lines in the southern solar hemisphere, from 1.5 to 5 R-s, were made with the SOHO Ultraviolet Coronagraph Spectrometer (UVCS) in May 2000 close to solar maximum. The ratio of the intensity of the two oxygen lines is used as a proxy for solar wind velocity in the inner corona. White light images of the corona taken with the SOHO/LASCO-C2 during the same time period, and used to place the UVCS observations in the context of coronal structures, show streamers extending to high latitudes. The measured radial and azimuthal gradients of the intensity ratio reflect strong velocity shears in the corona with the slowest wind coinciding with the axis of streamers. Comparison of these results with ratios measured with UVCS during solar minimum indicates that the transition from fast to slow wind in the inner corona occurs within 20 degrees of the axis of streamers at both phases of the solar cycle. C1 Univ Wales, Aberystwyth SY23 3BZ, Dyfed, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Paris 11, Inst Astrophys Spatiale, CNRS, F-91405 Orsay, France. RP Univ Wales, Aberystwyth SY23 3BZ, Dyfed, Wales. EM shabbal@cfa.harvard.edu; richard.woo@jpl.nasa.gov; vial@ias.fr NR 6 TC 3 Z9 3 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PY 2001 VL 97 IS 1-4 BP 5 EP 8 DI 10.1023/A:1011893104061 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 472DH UT WOS:000170967700002 ER PT J AU Woo, R Habbal, SR AF Woo, R Habbal, SR TI Associating the solar wind measured by Ulysses with its source at the sun SO SPACE SCIENCE REVIEWS LA English DT Review ID POLAR CORONAL HOLE; INTERPLANETARY SPACE; PLASMA OBSERVATIONS; PHYSICAL-PROPERTIES; DENSITY STRUCTURE; SOURCE REGIONS; SLOW; STREAMERS AB Radio occultation, ultraviolet, and white-light measurements have expanded our knowledge of the morphology of density and velocity in polar coronal holes, and made it possible to carry out the first systematic comparisons between the Ulysses solar wind measurements and quantitative white-light observations of the solar corona. This paper summarizes the rationale and salient features of this new approach which has been used to relate the solar wind observed by Ulysses in 1993-1995 to the inner corona. The statistical characteristics (average, standard deviation, and autocorrelation function) of the Ulysses density measurements of the fast wind are found to be mirrored in those of polarized brightness measurements of path-integrated density made by the High Altitude Observatory (HAO) Mauna Loa K-coronagraph at 1.15 R-circle dot. These results reinforce the conclusions from comparisons between measurements of the outer and inner corona. They show that the polar coronal hole extends radially into the solar wind, and that sources of the fast wind are not limited to coronal holes. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Wales, Aberystwyth, Dyfed, Wales. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 27 TC 2 Z9 2 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PY 2001 VL 97 IS 1-4 BP 81 EP 85 DI 10.1023/A:1011822010421 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 472DH UT WOS:000170967700016 ER PT B AU Smith, RK Brickhouse, NS Liedahl, DA Raymond, JC AF Smith, RK Brickhouse, NS Liedahl, DA Raymond, JC BE Ferland, G Savin, DW TI Standard formats for atomic data: the APED SO SPECTROSCOPIC CHALLENGES OF PHOTOIONIZED PLASMAS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Photoionized Plasmas 2000 Conference CY NOV 15-18, 2001 CL UNIV KENTUCKY, LEXINGTON, KY SP NASA Appl Informat Syst Res Program HO UNIV KENTUCKY ID PHOTOIONIZATION CROSS-SECTIONS; ELECTRON-IMPACT; EXCITATION; FITS; IONS AB Standardized formats for atomic data used in calculating emission from a collisionally-ionized plasma are described. The formats use the astronomical-standard FITS format, and are extendible to other purposes, such as photoionization data. The formats emphasize storing references to the original data source and keeping the data in as-received form, to aid in checking against the original literature. C1 Harvard Smithsonian Ctr Astrophys, High Energy Astrophys Div, Cambridge, MA 02138 USA. RP Smith, RK (reprint author), Harvard Smithsonian Ctr Astrophys, High Energy Astrophys Div, 60 Garden St, Cambridge, MA 02138 USA. NR 7 TC 32 Z9 32 U1 1 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-085-4 J9 ASTR SOC P PY 2001 VL 247 BP 161 EP 166 PG 6 WC Astronomy & Astrophysics; Optics; Physics, Fluids & Plasmas; Physics, Atomic, Molecular & Chemical; Spectroscopy SC Astronomy & Astrophysics; Optics; Physics; Spectroscopy GA BU54X UT WOS:000176291800016 ER PT S AU Adelberger, K AF Adelberger, K BE Tacconi, L Lutz, D TI The cosmic star-formation history: The UV finds most SO STARBURST GALAXIES: NEAR AND FAR, PROCEEDINGS SE SPRINGER PROCEEDINGS IN PHYSICS LA English DT Proceedings Paper CT Workshop on Starburst Galaxies: Near and Far CY SEP 10-15, 2000 CL RINGBERG CASTLE, GERMANY SP Max Planck Inst, Extraterrestr Phys ID ULTRAVIOLET LUMINOSITY DENSITY; HIGH-REDSHIFT; INFRARED GALAXIES; DUSTY; EVOLUTION C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Adelberger, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 18 TC 3 Z9 3 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0930-8989 BN 3-540-41472-X J9 SPRINGER PROC PHYS PY 2001 VL 88 BP 318 EP 327 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BT51L UT WOS:000173182100045 ER PT J AU Douglas, JG Chase, WT AF Douglas, JG Chase, WT TI Examination of two eastern Zhou jade and gold assemblages from Jincun, near Luoyang, Henan Province, China, and implications for the original configuration of the Freer Pectoral SO STUDIES IN CONSERVATION LA English DT Article AB In the light of recent archaeological finds in China, a jade and gold pectoral in the collection of the Freer Gallery of Art, dating to the Eastern Zhou dynasty, was examined to determine if its present configuration is correct. The pectoral consists of 10 jades attached to a linked gold chain, and is thought to come from the Eastern Zhou site of Jincun, near Luoyang, Henan Province, China. All 10 jades were found to have similar soil encrustations and similar major and minor elemental composition, as determined by X-ray fluorescence analysis. However, a scanning electron microscope (SEM_ study of the gold wires attaching the jades to the gold chain showed that four different types of wire were used. The Freer pectoral was found to be a reconfiguration of genuine jades on the gold chain, probably effected shortly after excavation in the late 1920s. The Freer pectoral was compared to another jade-and-gold necklace, also thought to be from the Eastern Zhou site of Jincun. The necklaces have different styles of chain, but both could have been made in China or the Western Steppes region in antiquity. C1 Smithsonian Inst, Freer Gallery Art Am Sackler Gallery, Dept Cosnervation & Sci Res, Washington, DC 20560 USA. Chase Art Services, Chevy Chase, MD 20815 USA. RP Douglas, JG (reprint author), Smithsonian Inst, Freer Gallery Art Am Sackler Gallery, Dept Cosnervation & Sci Res, Washington, DC 20560 USA. NR 18 TC 1 Z9 1 U1 0 U2 1 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0039-3630 EI 2047-0584 J9 STUD CONSERV JI Stud. Conserv. PY 2001 VL 46 IS 1 BP 35 EP 48 DI 10.2307/1506881 PG 14 WC Archaeology; Art; Chemistry, Applied; Chemistry, Analytical; Spectroscopy SC Archaeology; Art; Chemistry; Spectroscopy GA 436YT UT WOS:000168964000004 ER PT J AU Leona, M Winter, J AF Leona, M Winter, J TI Fiber optics reflectance spectroscopy: A unique tool for the investigation of Japanese paintings SO STUDIES IN CONSERVATION LA English DT Article AB Ultraviolet-visible reflectance spectroscopy is a rapid and accurate technique for the investigation of painted surfaces. The use of a high efficiency beveled-tip fiber optic probe and a pulsed xenon source gives improved detection efficiency and minimizes the interference from ambient light, eliminating the need to shield the analyzed area and allowing non-contact, non-invasive analysis. Thin washed of orgnaic colorants, often impossible to sample, are ideally suited to this kind of analysis. This study describes the in situ identification of indigo, Prussian blue and a red insect dye (cochineal carmine or lac dye) in two paintings by Katsushika Hokusai. C1 Los Angeles County Museum Art, Los Angeles, CA 90036 USA. Smithsonian Inst, Washington, DC 20560 USA. RP Leona, M (reprint author), Los Angeles County Museum Art, 5905 Wilshire Blvd, Los Angeles, CA 90036 USA. NR 27 TC 36 Z9 36 U1 1 U2 4 PU INT INST CONSERVATION HISTORIC ARTISTIC WORKS PI LONDON PA 6 BUCKINGHAM ST, LONDON, ENGLAND WC2N 6BA SN 0039-3630 J9 STUD CONSERV JI Stud. Conserv. PY 2001 VL 46 IS 3 BP 153 EP 162 DI 10.2307/1506806 PG 10 WC Archaeology; Art; Chemistry, Applied; Chemistry, Analytical; Spectroscopy SC Archaeology; Art; Chemistry; Spectroscopy GA 491EF UT WOS:000172094500001 ER PT B AU Aufdenberg, JP Hauschildt, PH Short, CI Starrfield, SG AF Aufdenberg, JP Hauschildt, PH Short, CI Starrfield, SG BE Woodward, CE Biscay, MD Shull, JM TI Optically thick winds of Novae SO TETONS 4: GALACTIC STRUCTURE, STARS, AND THE INTERSTELLAR MEDIUM SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Tetons Conference on Galactic Structure, Stars, and the Interstellar Medium CY MAY 28-JUN 01, 2000 CL GRAND TETON NATL PK, WY SP SIRFT C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Aufdenberg, JP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 15, Cambridge, MA 02138 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-064-1 J9 ASTR SOC P PY 2001 VL 231 BP 539 EP 540 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31M UT WOS:000175667600066 ER PT B AU Kenyon, SJ AF Kenyon, SJ BE Woodward, CE Biscay, MD Shull, JM TI Dynamical evolution of protoplanetary disks SO TETONS 4: GALACTIC STRUCTURE, STARS, AND THE INTERSTELLAR MEDIUM SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Tetons Conference on Galactic Structure, Stars, and the Interstellar Medium CY MAY 28-JUN 01, 2000 CL GRAND TETON NATL PK, WY SP SIRFT ID EDGEWORTH-KUIPER BELT; MAGNETOCENTRIFUGALLY DRIVEN FLOWS; SPECTRAL ENERGY-DISTRIBUTIONS; OUTER SOLAR-SYSTEM; PICTORIS DUST DISK; T-TAURI DISKS; BETA-PICTORIS; GIANT PLANETS; CIRCUMSTELLAR DISK; YOUNG STARS AB This paper reviews the theory of protostellar debris disks. After a brief introduction to accretion disk physics, I describe coagulation models of planet formation in the outer regions of planetesimal disks. Coagulation models for the Kuiper Belt produce Pluto-sized objects on timescales of 10-40 Myr. These models yield size distributions which agree with observations of Kuiper Belt objects with red magnitudes, R approximate to 20-27. Velocity stirring models for other debris disk systems demonstrate that 500 kin or larger objects can stir the velocities of small objects up to the shattering limit needed to begin a collisional cascade. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 156 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-064-1 J9 ASTR SOC P PY 2001 VL 231 BP 594 EP 619 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU31M UT WOS:000175667600076 ER PT J AU McDonnell, JT Platt, SR Clayton, LA AF McDonnell, JT Platt, SR Clayton, LA TI Neurologic conditions causing lameness in companion animals SO VETERINARY CLINICS OF NORTH AMERICA-SMALL ANIMAL PRACTICE LA English DT Article ID CAUDA-EQUINA SYNDROME; THORACOLUMBAR DISK EXTRUSION; NERVE SHEATH TUMOR; SPINAL-CORD TUMOR; LUMBOSACRAL STENOSIS; COMPUTED-TOMOGRAPHY; RETROSPECTIVE EVALUATION; SURGICAL-TREATMENT; BRACHIAL-PLEXUS; CERVICAL-SPINE AB Neurologic disease can cause lameness mimicking orthopedic disease in companion animals. This article presents a logical stepwise approach to help differentiate between orthopedic and neurologic causes of lameness. The neurologic examination, diagnostic techniques, and treatment options for these challenging cases are discussed. Specific diseases examined include myopathies, neuropathies, intervertebral disk disease, lumbosacral disease, peripheral nerve sheath tumors, spinal cord tumors, and traumatic neuropathies. C1 Tufts Univ, Sch Vet Med, Dept Clin Sci, N Grafton, MA 01536 USA. Anim Hlth Trust, Ctr Small Anim Studies, Newmarket, Suffolk, England. Smithsonian Natl Zoo Pk, Dept Anim Hlth, Washington, DC USA. RP McDonnell, JT (reprint author), Tufts Univ, Sch Vet Med, Dept Clin Sci, 200 Westboro Rd, N Grafton, MA 01536 USA. NR 64 TC 8 Z9 8 U1 0 U2 2 PU W B SAUNDERS CO PI PHILADELPHIA PA INDEPENDENCE SQUARE WEST CURTIS CENTER, STE 300, PHILADELPHIA, PA 19106-3399 USA SN 0195-5616 J9 VET CLIN N AM-SMALL JI Vet. Clin. N. Am.-Small Anim. Pract. PD JAN PY 2001 VL 31 IS 1 BP 17 EP + PG 23 WC Veterinary Sciences SC Veterinary Sciences GA 398AC UT WOS:000166730700003 PM 11787260 ER PT B AU Rots, A AF Rots, A BE Brunner, RJ Djorjovski, SG Szalay, AS TI The Chandra Data Archive SO VIRTUAL OBSERVATORIES OF THE FUTURE, PROCEEDINGS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Virtual Observatories of the Future CY JUN 13-16, 2000 CL CALIF INST TECHNOL, PASADENA, CA SP Natl Sci Fdn, Natl Aeronaut & Space Adm, Sun Microsyst & Microsoft Res HO CALIF INST TECHNOL ID AXAF AB We provide a quick overview of the design and usage attributes of the Chandra Data Archive. Its functional design incorporates a single observation database that controls the complete life cycle of all observations, The data products in the archive are mainly FITS files. Data distribution is expected to take place mainly through a web interface and FTP. We describe the archive access design and discuss the FITS conventions that were adopted for the data products. The time scale adopted for the data products is Terrestrial Time (TT). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rots, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-057-9 J9 ASTR SOC P PY 2001 VL 225 BP 209 EP 212 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS48T UT WOS:000170040800038 ER PT B AU Rots, A AF Rots, A BE Brunner, RJ Djorjovski, SG Szalay, AS TI The space-time profile for ISAIA SO VIRTUAL OBSERVATORIES OF THE FUTURE, PROCEEDINGS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Conference on Virtual Observatories of the Future CY JUN 13-16, 2000 CL CALIF INST TECHNOL, PASADENA, CA SP Natl Sci Fdn, Natl Aeronaut & Space Adm, Sun Microsyst & Microsoft Res HO CALIF INST TECHNOL AB We consider the problem of a user searching for observational information in a given region of the space-time universe where the user's specification may not match the coordinate systems used by all archives being browsed. We propose a draft profile to characterize the coordinate conventions used by both resource and query, allowing general coordinate transformations between what the seeker is looking for and what the resource has to offer. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rots, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-057-9 J9 ASTR SOC P PY 2001 VL 225 BP 213 EP 216 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS48T UT WOS:000170040800039 ER PT B AU Silver, S AF Silver, S BE Martin, V Sarathy, MAP TI Exploring sustainability in cocoa production: It's more than just about chocolate! SO WILDERNESS & HUMANITY: THE GLOBAL ISSUE LA English DT Proceedings Paper CT 6th World Wilderness Congress (WWC) CY 1998 CL BANGALORE, INDIA SP Thoresen Fdn, Ohrstrom Fdn, World Wilderness Trust, Wilderness Fdn, Wilderness Leadership Sch, Agromore Ltd, Armand G Erpf Fund, Govt Karnataka, Wild Fdn C1 Smithsonian Inst Yale Univ Liaison, Seattle, WA 98103 USA. NR 0 TC 0 Z9 0 U1 2 U2 4 PU FULCRUM PUBLISHING PI GOLDEN PA 16100 TABLE MT PKWY SUITE 300, GOLDEN, CO 80403 USA BN 1-55591-989-8 PY 2001 BP 246 EP 256 PG 11 WC Biodiversity Conservation; Environmental Sciences; Environmental Studies SC Biodiversity & Conservation; Environmental Sciences & Ecology GA BU37W UT WOS:000175847900041 ER PT S AU Elvis, M AF Elvis, M BE Czerny, B TI A wind origin for the reflection features in quasars SO X-RAY AND GAMMA-RAY SIGNATURES OF BLACK HOLES AND WEAKLY MAGNETIZED NEUTRON STARS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT E1 2/H0 3 Symposium of COSPAR Scientific Commission E held at the 33rd COSPAR Scientific Assembly CY JUL, 2000 CL WARSAW, POLAND SP Danish ID ACTIVE GALACTIC NUCLEI; SEYFERT-1 GALAXIES; ACCRETION DISK; COLD MATTER; SPECTRAL VARIABILITY; LINE REGION; BLACK-HOLE; NGC-5548; EMISSION; SPECTROPOLARIMETRY AB An alternative origin for the X-ray reflection features in quasar spectra is proposed. Unlike the relativistic disk model, the features axe formed in an accelerating wind at a relatively large distance from the central black hole. This wind model was developed to explain entirely other phenomena: the narrow and broad quasar absorption lines (NALs and BALs). The particular geometry and kinematics of the wind model also remove longstanding problems with having the quasar broad emission line region (BELR) gas be pressure confined. The wind has to be Compton thick along its flow direction, and this gives rise to a scattering and fluorescing region that must produce X-ray fluorescence and scattering features. Published by Elsevier Science Ltd on behalf of COSPAR. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 45 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0273-1177 J9 ADV SPACE RES PY 2001 VL 28 IS 2-3 BP 451 EP 457 DI 10.1016/S0273-1177(01)00435-5 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BT45X UT WOS:000173048700024 ER PT S AU Di Matteo, T AF Di Matteo, T BE White, NE Malaguti, G Palumbo, GGC TI Coronal heating and emission mechanisms in AGN SO X-RAY ASTRONOMY: STELLAR ENDPOINTS, AGN, AND THE DIFFUSE X-RAY BACKGROUND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Astronomy CY SEP 06-10, 1999 CL BOLOGNA, ITALY SP ITESRE CNR, NASA GSFC, ASI DE accretion, accretion disks; magnetic fields; radiation mechanisms : thermal; X-rays : general ID ACTIVE GALACTIC NUCLEI; ADVECTION-DOMINATED ACCRETION; DISKS AB Popular models for the formation of X-ray spectra in AGN assume that a large fraction of the disk's angular momentum dissipation takes place in a hot corona that carries a small amount of the accreting mass. Here I discuss the formation of a magnetically-structured accretion disk corona, generated by buoyancy instability in the disk and the heating of localized flare regions up to the canonical X-ray emitting temperatures. I also examine the analogy between accreting disk-coronae and ADAFs and discuss the relevant emission mechanism in these two accretion models and how observational constraints can allow us to discriminate between them. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Di Matteo, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 27 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0043-1 J9 AIP CONF PROC PY 2001 VL 599 BP 83 EP 92 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU03M UT WOS:000174772600008 ER PT S AU Kaaret, P AF Kaaret, P BE White, NE Malaguti, G Palumbo, GGC TI Spectral signatures of kilohertz quasi-periodic oscillations from accreting neutron stars SO X-RAY ASTRONOMY: STELLAR ENDPOINTS, AGN, AND THE DIFFUSE X-RAY BACKGROUND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Astronomy CY SEP 06-10, 1999 CL BOLOGNA, ITALY SP ITESRE CNR, NASA GSFC, ASI DE accretion, accretion disks; gravitation; relativity; stars : individual {4U 1820303); stars : neutron; X-rays : stars ID X-RAY BINARIES; SCORPIUS X-1; BLACK-HOLES; VARIABILITY; 4U-1820-30 AB Correlations discovered between millisecond timing properties and spectral properties in neutron star x-ray binaries are described and then interpreted in relation to accretion flows in the systems. Use of joint timing and spectral observations to test for the existence of the marginally stable orbit, a key prediction of strong field general relativity, is described and observations of the neutron star x-ray binary 4U 1820-303 which suggest that the signature of the marginally stable orbit has been detected are presented. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kaaret, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 23 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0043-1 J9 AIP CONF PROC PY 2001 VL 599 BP 179 EP 188 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU03M UT WOS:000174772600018 ER PT S AU Tananbaum, H AF Tananbaum, H BE White, NE Malaguti, G Palumbo, GGC TI Early results from the Chandra Observatory SO X-RAY ASTRONOMY: STELLAR ENDPOINTS, AGN, AND THE DIFFUSE X-RAY BACKGROUND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Astronomy CY SEP 06-10, 1999 CL BOLOGNA, ITALY SP ITESRE CNR, NASA GSFC, ASI DE X-rays : general; instrumentation : detectors and telescopes, Chandra C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tananbaum, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0043-1 J9 AIP CONF PROC PY 2001 VL 599 BP 387 EP 395 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU03M UT WOS:000174772600038 ER PT S AU Costantini, E Salvini, C Comastri, A Fruscione, A Mathur, S Nicastro, F Stirpe, GM Wilkes, B AF Costantini, E Salvini, C Comastri, A Fruscione, A Mathur, S Nicastro, F Stirpe, GM Wilkes, B BE White, NE Malaguti, G Palumbo, GGC TI The complex and variable absorption of NGC 3516 observed by BeppoSAX SO X-RAY ASTRONOMY: STELLAR ENDPOINTS, AGN, AND THE DIFFUSE X-RAY BACKGROUND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Astronomy CY SEP 06-10, 1999 CL BOLOGNA, ITALY SP ITESRE CNR, NASA GSFC, ASI DE AGN; X-ray spectroscopy; NGC 3516; BeppoSAX ID GALAXY AB We present 2 BeppoSAX (0.1-150 keV) observations of the Seyfert 1 galaxy NGC 3516, taken 4 months apart (8-11-1996, 12-03-1997). We find that during the 1996 observation the nuclear X-ray continuum was absorbed by an unusually large amount of cold gas clearly associated with the AGN environment. Unabsorbed thermal emission is also seen below 3 keV during this observation. Finally, the 0.1-10 keV spectra of both the observations show the presence of a complex system of ionized absorbing matter which we parameterize with two "warm absorber" with quite different degrees of ionization and column densities. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Costantini, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Stirpe, Giovanna/O-9393-2015; Comastri, Andrea/O-9543-2015; OI Stirpe, Giovanna/0000-0002-3702-8731; Comastri, Andrea/0000-0003-3451-9970; Wilkes, Belinda/0000-0003-1809-2364 NR 12 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0043-1 J9 AIP CONF PROC PY 2001 VL 599 BP 590 EP 593 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU03M UT WOS:000174772600080 ER PT S AU Kaaret, P Grindlay, J Lamb, FK Morgan, EH Swank, JH Zhang, W AF Kaaret, P Grindlay, J Lamb, FK Morgan, EH Swank, JH Zhang, W BE White, NE Malaguti, G Palumbo, GGC TI The relativistic astrophysics explorer: A new mission for X-ray timing SO X-RAY ASTRONOMY: STELLAR ENDPOINTS, AGN, AND THE DIFFUSE X-RAY BACKGROUND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Astronomy CY SEP 06-10, 1999 CL BOLOGNA, ITALY SP ITESRE CNR, NASA GSFC, ASI DE instrumentation : detectors; X-rays : general ID SPECTROSCOPY AB The great success of the Rossi X-Ray Timing Explorer (RXTE) has given us a new probe to study strong gravitational fields and to measure the physical properties of black holes and neutron stars. Here, we describe a "next-generation" x-ray timing mission, the Relativistic Astrophysics Explorer (RAE), designed to fit within the envelope of a "medium-sized" mission. The main instruments will be a narrow-field x-ray detector array with an area of at least 60,000 cm(2) equal to ten times that of RXTE, and a wide-field x-ray monitor with good sensitivity and few arcminute position resolution. We describe the design of the instruments and the science which will be possible with a factor of ten increase in collecting area. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kaaret, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Swank, Jean/F-2693-2012 NR 11 TC 5 Z9 5 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0043-1 J9 AIP CONF PROC PY 2001 VL 599 BP 678 EP 681 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU03M UT WOS:000174772600102 ER PT S AU Nicastro, F Elvis, M Fiore, F Matt, G Savaglio, S AF Nicastro, F Elvis, M Fiore, F Matt, G Savaglio, S BE White, NE Malaguti, G Palumbo, GGC TI High resolution observations of X-ray Absorbers/Emitters SO X-RAY ASTRONOMY: STELLAR ENDPOINTS, AGN, AND THE DIFFUSE X-RAY BACKGROUND SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Conference on X-Ray Astronomy CY SEP 06-10, 1999 CL BOLOGNA, ITALY SP ITESRE CNR, NASA GSFC, ASI DE AGN; ionized absorber; ionized emitter AB We present photoionization and collisional ionization models, and their application to three important fields: (a) the Warm Absorbers/Emitters in type 1 AGN, (b) the Warm Reflectors in Type 2 AGN, and (c) X-ray absorption of background quasars by intergalactic gas. A number of cases are investigated, and the dependences of the main parameters explored. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nicastro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 10 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0043-1 J9 AIP CONF PROC PY 2001 VL 599 BP 802 EP 805 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU03M UT WOS:000174772600133 ER PT B AU Tananbaum, H AF Tananbaum, H BE Giacconi, R Serio, S Stella, L TI Chandra overview SO X-RAY ASTRONOMY 2000 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT X-Ray Astronomy 2000 Conference CY SEP 04-09, 2000 CL MONDELLO, ITALY SP Soc Astron Italiana, Agenzia Spaziale Italiana, Citta Palermo, Compaq, CNR, Makers, Prov Reg Palermo, Reg Sicilia, Telecom Italia, Univ Studi Palermo AB The third of NASA's four Great Observatories, the Chandra X-ray Observatory, was launched aboard the Shuttle Columbia on July 23, 1999. Using an Inertial Upper Stage and an internal propulsion system, Chandra was raised to a highly elliptical orbit ranging from 10,000 km to 140,000 km. After a successful activation of all spacecraft, telescope, and science instrument systems, Chandra began observing celestial targets about 1 month after launch. From the start, Chandra has provided spectacular images and spectra for essentially all types of astronomical objects including stars, supernova remnants, normal and active galaxies, and clusters of galaxies. The Observatory status and selected science highlights are presented here. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tananbaum, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 11 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-071-4 J9 ASTR SOC P PY 2001 VL 234 BP 3 EP 14 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU25U UT WOS:000175482700001 ER PT B AU Drake, JJ AF Drake, JJ BE Giacconi, R Serio, S Stella, L TI Stellar coronae: The first 25 years SO X-RAY ASTRONOMY 2000 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT X-Ray Astronomy 2000 Conference CY SEP 04-09, 2000 CL MONDELLO, ITALY SP Soc Astron Italiana, Agenzia Spaziale Italiana, Citta Palermo, Compaq, CNR, Makers, Prov Reg Palermo, Reg Sicilia, Telecom Italia, Univ Studi Palermo ID X-RAY-EMISSION; SOLAR-TYPE STARS; UX ARIETIS; ROTATION; MASS; ABUNDANCES; EINSTEIN; SYSTEMS; DWARFS; FLARES AB Hot X-ray emitting coronae were detected on stars other than the Sun about twenty five years ago. This review describes some of the observational advances that have improved our knowledge of stellar coronae, with an emphasis toward understanding the more active stars. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS-3,60 Garden St, Cambridge, MA 02138 USA. EM jdrake@cfa.harvard.edu NR 43 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-071-4 J9 ASTR SOC P PY 2001 VL 234 BP 53 EP 64 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU25U UT WOS:000175482700005 ER PT B AU Fabbiano, G AF Fabbiano, G BE Giacconi, R Serio, S Stella, L TI First Chandra observations of galaxies SO X-RAY ASTRONOMY 2000 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT X-Ray Astronomy 2000 Conference CY SEP 04-09, 2000 CL MONDELLO, ITALY SP Soc Astron Italiana, Agenzia Spaziale Italiana, Citta Palermo, Compaq, CNR, Makers, Prov Reg Palermo, Reg Sicilia, Telecom Italia, Univ Studi Palermo ID ROSAT-PSPC OBSERVATIONS; ELLIPTIC GALAXIES; ANTENNAE GALAXIES; M31; NGC-4038/4039; EMISSION; ASCA AB Chandra's unique combination of sub-arcsecond angular resolution and spectral resolution is very well suited to the study of complex X-ray emitting systems, such as galaxies. In this talk, I give an overview of very early results on galaxies, including examples of normal spirals (M31, M33, M81 and M83), the actively star-forming merging galaxy pair NGC 4038/39 (the Antennae), and the nearby active SO galaxy NGC 5128 (Centaurus A). In all cases, we can easily discriminate between the emission from a population of individual X-ray sources, hot ISM components, and nuclear sources, when present. Highlights of these early results include the detection of a rich population of X-ray sources in nearby galaxies of all morphological types, including the detection of the debated population of XRBs in in the SO NGC 5128; the detection of super-luminous (super-Eddington) sources in the Antennae galaxies, whose counterpart may be intermediate mass black holes (10-100s M(circle dot)); and the detection of a whole range of features in the hot ISM. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 35 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-071-4 J9 ASTR SOC P PY 2001 VL 234 BP 295 EP 306 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU25U UT WOS:000175482700035 ER PT B AU Mahdavi, A Bohringer, H Geller, MJ Ramella, M AF Mahdavi, A Bohringer, H Geller, MJ Ramella, M BE Giacconi, R Serio, S Stella, L TI The RASSCALS: An X-ray and optical study of 260 galaxy groups SO X-RAY ASTRONOMY 2000 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT X-Ray Astronomy 2000 Conference CY SEP 04-09, 2000 CL MONDELLO, ITALY SP Soc Astron Italiana, Agenzia Spaziale Italiana, Citta Palermo, Compaq, CNR, Makers, Prov Reg Palermo, Reg Sicilia, Telecom Italia, Univ Studi Palermo AB The ROSAT All-Sky Survey-Center for Astrophysics Loose Systems (RASSCALS) are the largest redshift-selected catalog of low mass galaxy groups to date, covering 1/4 of the sky in the 0.01 < z < 0.04 universe. I describe the distribution of the RASSCALS within the nearby large scale structure, examine their X-ray and optical scaling laws, and describe recent results from a deep redshift survey in the direction of the X-ray emitting systems. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mahdavi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 10, Cambridge, MA 02138 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-071-4 J9 ASTR SOC P PY 2001 VL 234 BP 411 EP 416 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU25U UT WOS:000175482700051 ER PT B AU Schwartz, DA Elvis, M Harris, DE Hooper, EJ Tucker, WH Virani, S Wilkes, B Marshall, HL Lovell, JEJ Tingay, SJ Jauncey, DL Piner, BG Preston, RA Birkinshaw, M Worrall, DM Chartas, G Feigelson, ED Ghosh, KK Hirabayashi, H Lanzetta, KM Mathur, S AF Schwartz, DA Elvis, M Harris, DE Hooper, EJ Tucker, WH Virani, S Wilkes, B Marshall, HL Lovell, JEJ Tingay, SJ Jauncey, DL Piner, BG Preston, RA Birkinshaw, M Worrall, DM Chartas, G Feigelson, ED Ghosh, KK Hirabayashi, H Lanzetta, KM Mathur, S BE Giacconi, R Serio, S Stella, L TI Chandra observations of the PKS 0637-752 X-ray jet SO X-RAY ASTRONOMY 2000 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT X-Ray Astronomy 2000 Conference CY SEP 04-09, 2000 CL MONDELLO, ITALY SP Soc Astron Italiana, Agenzia Spaziale Italiana, Citta Palermo, Compaq, CNR, Makers, Prov Reg Palermo, Reg Sicilia, Telecom Italia, Univ Studi Palermo ID PKS-0637-752 AB We previously have discussed the discovery of a luminous X-ray jet coincident with the inner western radio jet of the PKS 0637-752 system. Here we report the detection of very weak X-ray emissions coincident with the eastern radio spot, and associated with the northwest extension of the radio jet. The HST image shows that many faint galaxies are surrounding the quasar PKS 0637-752. After deriving a mirror scattering function, we place an upper limit of 6 x 10(43) ergs s(-1) to X-ray emission from a possible cluster of galaxies at this location. The cluster gas pressure is negligible, except possibly for a highly relativistic jet. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schwartz, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Tingay, Steven/B-5271-2013 NR 8 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-071-4 J9 ASTR SOC P PY 2001 VL 234 BP 493 EP 499 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU25U UT WOS:000175482700062 ER PT B AU Nicastro, F Fruscione, A Elvis, M Siemiginowska, A Fiore, F Bianchi, S AF Nicastro, F Fruscione, A Elvis, M Siemiginowska, A Fiore, F Bianchi, S BE Giacconi, R Serio, S Stella, L TI The Chandra high resolution spectra of Mkn 421 SO X-RAY ASTRONOMY 2000 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT X-Ray Astronomy 2000 Conference CY SEP 04-09, 2000 CL MONDELLO, ITALY SP Soc Astron Italiana, Agenzia Spaziale Italiana, Citta Palermo, Compaq, CNR, Makers, Prov Reg Palermo, Reg Sicilia, Telecom Italia, Univ Studi Palermo ID LY-ALPHA FOREST AB Mkn 421 was observed by Chandra twice, on November 5, 1999 as part of the Chandra calibration program, with the ACIS-HETG configuration, and on May 29, 2000 following our Target Of Opportunity request aimed to caught the source in an ultra-high state, with both the ACIS-HETG and the HRC-LETG configurations. In this contribution we present and compare the two Chandra-MEG observations of Mkn 421, which lasted 26 and 19.6 ks respectively. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nicastro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 10 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-071-4 J9 ASTR SOC P PY 2001 VL 234 BP 511 EP 516 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU25U UT WOS:000175482700064 ER PT B AU Schnopper, H Silver, E Murray, S Jones, C Forman, W Bandler, S Romaine, S Slane, P Grindlay, J Madden, N Beeman, J Haller, E Smith, D Barbera, M Collura, A Christensen, F Ramsey, B Woosley, S Diehl, R Tucker, G Fabregat, J Reglero, V Gimenez, A AF Schnopper, H Silver, E Murray, S Jones, C Forman, W Bandler, S Romaine, S Slane, P Grindlay, J Madden, N Beeman, J Haller, E Smith, D Barbera, M Collura, A Christensen, F Ramsey, B Woosley, S Diehl, R Tucker, G Fabregat, J Reglero, V Gimenez, A BE Giacconi, R Serio, S Stella, L TI B-MINE: Balloon-borne microcalorimeter nuclear line explorer SO X-RAY ASTRONOMY 2000 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT X-Ray Astronomy 2000 Conference CY SEP 04-09, 2000 CL MONDELLO, ITALY SP Soc Astron Italiana, Agenzia Spaziale Italiana, Citta Palermo, Compaq, CNR, Makers, Prov Reg Palermo, Reg Sicilia, Telecom Italia, Univ Studi Palermo ID SUPERNOVA REMNANT; TI-44; EMISSION C1 Smithsonian Astrophys Observ, Cambridge, MA USA. RP Schnopper, H (reprint author), Smithsonian Astrophys Observ, Cambridge, MA USA. RI Bandler, Simon/A-6258-2010; Fabregat, Juan/F-9066-2016 OI Bandler, Simon/0000-0002-5112-8106; Fabregat, Juan/0000-0002-5986-9347 NR 22 TC 1 Z9 1 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-071-4 J9 ASTR SOC P PY 2001 VL 234 BP 633 EP 645 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU25U UT WOS:000175482700079 ER PT B AU Silver, E Schnopper, H Bandler, S Brickhouse, N Murray, S Barbera, M Takacs, E Gillaspy, JD Porto, JV Kink, I Deslattes, R Hudson, L Laming, JM AF Silver, E Schnopper, H Bandler, S Brickhouse, N Murray, S Barbera, M Takacs, E Gillaspy, JD Porto, JV Kink, I Deslattes, R Hudson, L Laming, JM BE Giacconi, R Serio, S Stella, L TI Laboratory astrophysics using a micro calorimeter on an Electron Beam Ion Trap SO X-RAY ASTRONOMY 2000 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT X-Ray Astronomy 2000 Conference CY SEP 04-09, 2000 CL MONDELLO, ITALY SP Soc Astron Italiana, Agenzia Spaziale Italiana, Citta Palermo, Compaq, CNR, Makers, Prov Reg Palermo, Reg Sicilia, Telecom Italia, Univ Studi Palermo ID LINE AB Cosmic plasma conditions created in an Electron Beam Ion Trap (EBIT) make it possible to simulate the dependencies of key diagnostic x-ray lines on density, temperature, and excitation conditions that exist in astrophysical sources. We used a microcalorimeter to measure broad band spectra obtained from the NIST EBIT with an energy resolution approaching that of a Bragg crystal spectrometer. Spectra are presented for nitrogen, oxygen, neon, argon, and iron in various stages of ionization. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Silver, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Bandler, Simon/A-6258-2010 OI Bandler, Simon/0000-0002-5112-8106 NR 13 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-071-4 J9 ASTR SOC P PY 2001 VL 234 BP 647 EP 656 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU25U UT WOS:000175482700080 ER PT J AU Kaeppler, AL AF Kaeppler, AL TI Dance and the concept of style SO YEARBOOK FOR TRADITIONAL MUSIC LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. RP Kaeppler, AL (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 12 TC 6 Z9 6 U1 0 U2 0 PU INT COUNCIL TRADITIONAL MUSIC PI LOS ANGELES PA UCLA/DEPT ETHNOMUSICOLOGY, 2539 SCHOENBERG, BOX 957178, LOS ANGELES, CA 90095 USA SN 0740-1558 J9 YEARB TRADIT MUSIC JI Yearb. Tradit. Mus. PY 2001 VL 33 BP 49 EP 63 DI 10.2307/1519630 PG 15 WC Music SC Music GA 656JK UT WOS:000181604500005 ER PT B AU Luhman, KL AF Luhman, KL BE Jayawardhana, R Greeme, TP TI On the MBM12 young association SO YOUNG STARS NEAR EARTH: PROGRESS AND PROSPECTS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Young Stars Near Earth CY MAR 28-30, 2001 CL NASA AMES RES CTR, MT VIEW, CA SP NASA Off Space Sci HO NASA AMES RES CTR ID LOW-MASS STARS; T-TAURI STARS; BROWN DWARFS; SPECTROSCOPY; CLOUDS AB I briefly describe the results of a comprehensive study of the MBM12 young association (MBM12A). I have obtained RI images of a 1.75degrees x 1.4degrees field encompassing most of the MBM12 dark cloud, combined these data with IR photometry from the Two-Micron All-Sky Survey (2MASS), and obtained optical spectroscopy of the resulting candidate members of the association. I find five new members with masses of 0.1-0.4 AI(E), where this census is complete to 0.02 M-circle dot. If the mass function in MBM12A were the same as that in the Trapezium Cluster (Luhman et al.), 3-4 brown dwarfs (> 0.02 M-circle dot) are experted in MBM12A where none are found. From an analysis of optical and IR photometry for Stars projected against the cloud, I identify M dwarfs in the foreground and background of the cloud. By comparing their magnitudes to those of local field dwarfs, I arrive at a distance modulus 7.2 +/- 0.5 (275 pc) for the MBM12 cloud. Thus. MBM12 is not the nearest molecular cloud and is not inside the local bubble of hot ionized gas as had been implied by previous distance estimates of 50-100 pc. In addition, I have used Li strengths and H-R diagrams to constrain the absolute and relative ages of MBM12A and other young populations; these data indicate ages of 2 Myr for MBM12A (for 275 pc.) and 10 Myr for the TW Hya and eta Cha associations. Various properties of MBM12A suggest that it is a slightly evolved version of the aggregates of young stars within the Taurus dark clouds (similar to1 Myr). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-082-X J9 ASTR SOC P PY 2001 VL 244 BP 26 EP 31 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU34B UT WOS:000175724200005 ER PT B AU van den Ancker, ME Perez, MR de Winter, D AF van den Ancker, ME Perez, MR de Winter, D BE Jayawardhana, R Greeme, TP TI The young stellar group associated with HD 199143 SO YOUNG STARS NEAR EARTH: PROGRESS AND PROSPECTS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Young Stars Near Earth CY MAR 28-30, 2001 CL NASA AMES RES CTR, MT VIEW, CA SP NASA Off Space Sci HO NASA AMES RES CTR ID STAR-FORMATION; IDENTIFICATION AB Recently, several groups of young stars in the solar neighborhood have been discovered. Given their proximity, these systems are ideally suited for detailed studies of star and planet formation. Here we report on a group of young stars associated with the bright F8V star HD 199143. At a distance of only 48 pc, this is the closest YSO group containing a classical T Tauri star (HD,358623; K7-M0e). New ground-based mid-infrared data shows that both HD 199143 and HD 358623 have large infrared excesses due to circumstellar disks. A systematic search for new members of this Capricornius association has yielded four new probable members, which we use to derive an age of 5-10 Mlyr for the group as a whole. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van den Ancker, ME (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. NR 7 TC 7 Z9 7 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-082-X J9 ASTR SOC P PY 2001 VL 244 BP 69 EP 74 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU34B UT WOS:000175724200013 ER PT B AU Wolk, SJ Smith, R Plucinsky, P Edgar, R Spitzbart, B Jayawardhana, R Hearty, TJ AF Wolk, SJ Smith, R Plucinsky, P Edgar, R Spitzbart, B Jayawardhana, R Hearty, TJ BE Jayawardhana, R Greeme, TP TI X-ray sources in the nearby star forming cloud, MBM 12 SO YOUNG STARS NEAR EARTH: PROGRESS AND PROSPECTS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Young Stars Near Earth CY MAR 28-30, 2001 CL NASA AMES RES CTR, MT VIEW, CA SP NASA Off Space Sci HO NASA AMES RES CTR ID MOLECULAR CLOUD AB The MBM 12 cloud is suspected to be the youngest near-by star forming cloud. We observed the densest part of this cloud for about 100 ks using the Chandra X-ray Observatory. We have detected 23 point sources in cloud. All the sources are fairly hard due to the extinction of the cloud. However after compensating for the extinction, up to 1/2 of the sources have hardness consistent with a coronal source. One source is coincident with a radio bright CO clump. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-082-X J9 ASTR SOC P PY 2001 VL 244 BP 165 EP 170 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU34B UT WOS:000175724200028 ER PT B AU Wilner, DJ AF Wilner, DJ BE Jayawardhana, R Greeme, TP TI Millimeter observations of the TW Hya system SO YOUNG STARS NEAR EARTH: PROGRESS AND PROSPECTS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Young Stars Near Earth CY MAR 28-30, 2001 CL NASA AMES RES CTR, MT VIEW, CA SP NASA Off Space Sci HO NASA AMES RES CTR ID TAURI STARS; DISK; HYDRAE AB We present millimeter wavelength aperture synthesis observations of TW Hya obtained with the Very Large Array and the BIMA array. Images at 7 mm resolve the dusty circumstellar disk surrounding the star, probing structure to size scales of 0."1 (similar to5AU). We describe how the long wavelength spectrum and resolved millimeter images constrain the radial distribution of disk surface density. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wilner, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 6 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-082-X J9 ASTR SOC P PY 2001 VL 244 BP 191 EP 196 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU34B UT WOS:000175724200032 ER PT B AU Torres, G Neuhauser, R Latham, DW AF Torres, G Neuhauser, R Latham, DW BE Jayawardhana, R Greeme, TP TI Radial-velocity monitoring of members and candidate members of the TW Hydrae association SO YOUNG STARS NEAR EARTH: PROGRESS AND PROSPECTS SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Workshop on Young Stars Near Earth CY MAR 28-30, 2001 CL NASA AMES RES CTR, MT VIEW, CA SP NASA Off Space Sci HO NASA AMES RES CTR ID SPECTROSCOPIC BINARIES; TODCOR; STARS AB We present our spectroscopic measurements of the radial velocity, effective temperature, and projected rotational velocity of several of the known members of the TW Hya association, as well as measurements for candidate members selected on the basis of their X-ray or kinematic properties. A number of our targets turn out to be binaries, but most are non-members. The radial velocities for some of the other candidates support the conclusion that they are kinematically associated with the group, although further observations are required to show that they are indeed pre-main sequence objects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St Mail Stop 20, Cambridge, MA 02138 USA. NR 9 TC 10 Z9 10 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 1-58381-082-X J9 ASTR SOC P PY 2001 VL 244 BP 283 EP 288 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BU34B UT WOS:000175724200047 ER PT S AU Schlegel, EM AF Schlegel, EM BE Holt, SS Hwang, U TI Early optical spectroscopic evidence for conical ejection in supernovae? SO YOUNG SUPERNOVA REMNANTS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 11th Annual Astrophysics Conference CY OCT 16-18, 2000 CL COLLEGE PK, MD AB We suggest that a parabolic emission feature observed in the optical spectra of several recent supernovae indicates the conical ejection of matter. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schlegel, EM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 16 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0001-6 J9 AIP CONF PROC PY 2001 VL 565 BP 69 EP 72 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS29B UT WOS:000169367800006 ER PT S AU Eriksen, KA Morse, JA Kirshner, RP Winkler, PF AF Eriksen, KA Morse, JA Kirshner, RP Winkler, PF BE Holt, SS Hwang, U TI Fabry-Perot [O III] lambda 5007 angstrom observations of the SMC oxygen-rich SNR 1E 0102-72.9 SO YOUNG SUPERNOVA REMNANTS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 11th Annual Astrophysics Conference CY OCT 16-18, 2000 CL COLLEGE PK, MD ID SUPERNOVA REMNANT; MAGELLANIC CLOUD; 1E-0102.2-7219; N132D; YOUNG AB We present Rutgers/CTIO Fabry-Perot Imaging Spectrometer observations of the [O III] 5007 Angstrom line of the oxygen-rich supernova remnant 1E 0102-72.9 in the Small Magellanic Cloud. Our data cube covers velocities from -2100 km/s to +2300 km/s with 100 km/s resolution, and for the first time reveals the complex three-dimensional structure of this remnant. The most prominent features are a number of rings of emission that are continuous in (X, Y, V) space, and bear striking resemblance to the Fe-Ni bubbles studied in recent numerical models. Using a simple kinematic model, we derive a free expansion age of 2100 years for E0102. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Eriksen, KA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 10 Z9 10 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0001-6 J9 AIP CONF PROC PY 2001 VL 565 BP 193 EP 196 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS29B UT WOS:000169367800026 ER PT S AU Slane, P Hughes, JP Edgar, RJ Plucinsky, PP Miyata, E Tsunemi, H Aschenbach, B AF Slane, P Hughes, JP Edgar, RJ Plucinsky, PP Miyata, E Tsunemi, H Aschenbach, B BE Holt, SS Hwang, U TI Nonthermal X-ray emission from G266.2-1.2 (RX J0852.0-4622) SO YOUNG SUPERNOVA REMNANTS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 11th Annual Astrophysics Conference CY OCT 16-18, 2000 CL COLLEGE PK, MD ID VELA SUPERNOVA REMNANT; DISCOVERY; SHELL AB The newly discovered supernova remnant G266.2-1.2 (RX J0852.0 4622), along the line of sight to the Vela SNR, was observed with ASCA for 120 ks. We find that the X-ray spectrum is featureless, and well described by a power law, extending to three the class of shell-type SNRs dominated by nonthermal X-ray emission. Although the presence of the Vela SNR compromises our ability to accurately determine the column density, the GIS data appear to indicate absorption considerably in excess of that for Vela itself, indicating that G266.2-1.2 may be several times more distant. An unresolved central source may be an associated neutron star, though difficulties with this interpretation persist. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 14 TC 4 Z9 4 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0001-6 J9 AIP CONF PROC PY 2001 VL 565 BP 403 EP 406 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BS29B UT WOS:000169367800061 ER PT J AU Moreira, N Monteiro-Filho, ELA Moraes, W Swanson, WF Graham, LH Pasquali, OL Gomes, MLF Morais, RN Wildt, DE Brown, JL AF Moreira, N Monteiro-Filho, ELA Moraes, W Swanson, WF Graham, LH Pasquali, OL Gomes, MLF Morais, RN Wildt, DE Brown, JL TI Reproductive steroid hormones and ovarian activity in felids of the Leopardus genus SO ZOO BIOLOGY LA English DT Article DE fecal steroids; estrogens; progestogens; non-invasive monitoring; estrous cycle; reproduction; ovarian activity ID SEXUAL-BEHAVIOR; DOMESTIC CAT; PROGESTERONE; ESTRADIOL-17-BETA; PLASMA AB Reproductive endocrine patterns were characterized in female ocelots (Leopardus pardalis; n = 3), tigrinas (Leopardus tigrinus; n = 2), and margays (Leopardus wiedii; n = 2) housed in captivity in southern Brazil. Females were maintained as singletons and exposed to natural fluctuations in photoperiod. Cyclic changes in ovarian steroids were monitored by analyzing estrogen and progestogen metabolites in fecal samples collected five times weekly far 14 to 18 months. Based on intervals between fecal estrogen peaks, mean (+/- SEM) duration of the estrous cycle was 18.4 +/- 1.6 days for the ocelots (range, 7-31 days; n = 75 cycles), 16.7 +/- 1.3 days for the tigrinas (range, 11-27 days; n = 23 cycles), and 17.6 +/- 1.5 days for the margays (range, 11-25 days; n = 32 cycles). Fecal progestogen analyses combined with two laparoscopic observations of the ovaries confirmed that ocelots and tigrinas did not ovulate spontaneously. In contrast, non-mating-induced luteal phases of 40.1 +/- 6.3 days in duration (range, 30-60 days) were observed frequently in both margays. There was no evidence of gonadal seasonality in margays in either follicular or luteal activity. In ocelots, cyclic changes in estrogen excretion were observed during each month of the year; however, only one female cycled continuously. In the other two ocelots, periods of acyclicity of several months' duration were observed. It was not possible to conclude whether tigrinas were aseasonal because estrous cyclicity was observed in only one of two individuals. In the female that cycled, a 3-month period of acyclicity was observed in the late fall/early winter. These data demonstrate similarities among three felid species of the genus Leopardus, including evidence they are polyestrous but experience unexplained periods of ovarian inactivity. Only the margays differed by exhibiting occasional spontaneous, non-mating-induced ovulations. Historically, these species have not bred well in captivity. However, it is hoped that understanding the biological similarities and differences among them could lead to improved management strategies that may one day result in increased reproductive success. (C) 2001 Wiley-Liss. Inc. C1 Univ Fed Parana, Curso Med Vet, Dept Physiol, Zool Post Grad Course, BR-85950000 Palotina, Parana, Brazil. Univ Fed Parana, Zool Post Grad Course, Dept Zool, BR-80060000 Curitiba, Parana, Brazil. Itaipu Binacional, Foz Iguassu, Parana, Brazil. Cincinnati Zoo & Bot Garden, Ctr Res Endangered Wildlife, Cincinnati, OH USA. Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. Zool Curitiba, Curitiba, Parana, Brazil. Univ Fed Parana, Dept Physiol, BR-80060000 Curitiba, Parana, Brazil. RP Moreira, N (reprint author), Univ Fed Parana, Curso Med Vet, Dept Physiol, Zool Post Grad Course, Rua 24 Junho,698,Palotina Campus, BR-85950000 Palotina, Parana, Brazil. RI Moreira, Nei/C-6399-2013; Monteiro-Filho, Emygdio/C-7165-2013; Morais, Rosana/R-4928-2016 OI Moreira, Nei/0000-0002-9236-667X; Morais, Rosana/0000-0002-0816-4371 NR 30 TC 72 Z9 75 U1 4 U2 26 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 2001 VL 20 IS 2 BP 103 EP 116 DI 10.1002/zoo.1010 PG 14 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 447AK UT WOS:000169546200004 ER PT J AU Brown, JL Bellen, AC Fouraker, M Wildt, DE Roth, TL AF Brown, JL Bellen, AC Fouraker, M Wildt, DE Roth, TL TI Comparative analysis of gonadal and adrenal activity in the black and white rhinoceros in North America by noninvasive endocrine monitoring SO ZOO BIOLOGY LA English DT Article DE Ceratotherium simum; Diceros bicornis; fecal steroids; progestogens; estrogens; corticoids; androgens; ovarian activity; pregnancy; testicular activity; adrenal activity ID CERATOTHERIUM-SIMUM-SIMUM; FECAL STEROID ANALYSIS; DICEROS-BICORNIS; ESTROUS-CYCLE; PREGNANCY; BEHAVIOR; ESTROGENS; PROGESTERONE; METABOLISM; DIAGNOSIS AB Patterns of fecal reproductive steroid metabolites and adrenal corticoids were characterized for 12- to 24-month periods in black (n = 10 male, 16 female) and white (n = 6 male, 13 female) rhinoceroses at 14 institutions. All black rhinoceros females exhibited at least some ovarian cyclicity on the basis of fecal progestogen analysis (range, 2-12 cycles/yr). However, cycles often were erratic, with many being shorter (<20 days; 18% of cycles) or longer (>32 days; 21%) than the average of 26.8 +/- 0.5 days (n = 104 cycles). Five females exhibited periods of acyclicity of 2-10-month duration that were unrelated to season. One complete and seven partial pregnancies were evaluated in the black rhinoceros. Fecal progestogens increased over luteal phase concentrations after 3 months of gestation. Females resumed cyclicity within 3 months postpartum, before calves were weaned (n = 5). Approximately half of white rhinoceros females (6 of 13) showed no evidence of ovarian cyclicity. Of the cycles observed, 5 were "short" (32.8 +/- 1.2 days) and 24 were "long" (70.1 +/- 1.6 days). Only two females cycled continuously throughout the study. One had both long (n = 9) and short (n = 2) cycles, whereas the other exhibited long cycles only (n = 5). Fecal estrogen excretion was variable, and profiles were not useful for characterizing follicular activity or diagnosing pregnancy in either species. Males of both species showed no evidence of seasonality on the basis of fecal androgen profiles. Androgen metabolite concentrations were higher (P < 0.05) in the black (27.6 < 6.9 ng/g) than in the white (16.8 < 3.1 ng/g) rhinoceros. An adrenocorticotropin hormone challenge in four black rhinoceros males demonstrated that the clearance rate of corticoid metabolites into feces was similar to24 hours. Fecal corticoid concentrations did not differ between males and females, but overall means were higher in the black (41.8 +/- 3.1 ng/g) than in the white (31.2 +/- 1.7 ng/g) rhinoceros. In summary, fecal steroid analysis identified a number of differences in hormonal secretory dynamics between the black and white rhinoceros that may be related to differences in reproductive rates in captivity. Most black rhinoceros females exhibited some cyclic ovarian activity. In contrast, few white rhinoceroses demonstrated evidence of regular estrous cyclicity, and those females that were active had comparatively long cycles. Results also suggest that fecal corticoid concentrations reflect adrenal activity and may be species specific. Continued studies are needed to determine whether fecal corticoid measurements will be useful for understanding the cause of inconsistent gonadal activity in these two species. Because all but three (15.8%) of the white rhinoceroses evaluated in this study were less than 20 years of age compared to 73.1% (19 of 26) of the black rhinoceroses, the impact of age on reproductive and adrenal activity also needs to be evaluated further, (C) 2002 Wiley-Liss, Inc. C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. Fort Worth Zoo, Ft Worth, TX USA. Cincinnati Zoo & Bot Garden, Ctr Res Endangered Wildlife, Cincinnati, OH USA. RP Brown, JL (reprint author), Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. NR 35 TC 56 Z9 59 U1 1 U2 7 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 2001 VL 20 IS 6 BP 463 EP 486 DI 10.1002/zoo.10028 PG 24 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 532WD UT WOS:000174497300002 ER PT J AU Young, KM Brown, JL Goodrowe, KL AF Young, KM Brown, JL Goodrowe, KL TI Characterization of reproductive cycles and adrenal activity in the black-footed ferret (Mustela nigripes) by fecal hormone analysis SO ZOO BIOLOGY LA English DT Article DE feces; estradiol; progestins; pregnancy; pseudopregnancy; corticoids; restraint ID MONITORING OVARIAN-FUNCTION; CHEETAH ACINONYX-JUBATUS; ADRENOCORTICAL FUNCTION; PLASMA PROGESTERONE; ENZYME-IMMUNOASSAY; ESTROUS BEHAVIOR; LYCAON-PICTUS; DOMESTIC CAT; PREGNANCY; STRESS AB The reproductive cycle of the black-footed ferret (Mustela nigripes) was characterized by enzyme immunoassay (EIA) analysis of ovarian fecal steroids (estradiol, progestins) in 29 females over two consecutive breeding seasons. Estrous status was determined by measuring the vulva size and examining the percentage of superficial cells in vaginal lavages. Mean fecal estradiol concentrations were correlated with vulval area (r = 0.370, P < 0.0001) and the percentage of superficial cells (r = 0.380, P < 0.0001). Ovulation resulted in a rise in fecal progestin concentrations 5 days after breeding that differed (P < 0.05) between pregnant (n = 14) and pseudopregnant (n = 12) females during the late luteal phase (days 12-40), with concentrations remaining higher in pregnant animals. Gestation length was 41.3 +/- 0.7 days with 3.6 +/- 0.4 kits produced per female. Litter size correlated significantly (P < 0.05) with fecal estradiol, but not progestins during the 12 to 40 days after breeding. Females failing to breed (n = 3) remained in estrus for 31 +/- 6.2 days before ovulation induction with human chorionic gonadotropin. Adrenal activity in male (n = 4) and female (n = 6) black-footed ferrets was monitored by quantifying fecal corticoid metabolites after a series of manipulations (physical restraint, intramuscular saline, intramuscular gel adrenocorticotropic hormone (ACTH), intramuscular liquid ACTH). A significant (P < 0.0001) increase in fecal corticoids above the pre-treatment baseline occurred 20 to 44 hours after restraint (five of 10 animals), saline (six of nine), gel ACTH (seven of 10), and liquid ACTH (nine of 10) treatments. Immunoreactivity of high-performance liquid chromatography-separated fecal elutes was compared using antibodies against cortisol and corticosterone. The cortisol EIA demonstrated immunoreactivity that co-eluted with H-3-cortisol, whereas a corticosterone radioimmunoassay detected a metabolite peak that coeluted with H-3-corticosterone in addition to a slightly less polar and one considerably more polar peak. Despite recognizing different metabolites, both assays produced similar temporal profiles of corticoid excretion after manipulation. This study provides new information on the black-footed ferret regarding differences in fecal steroid excretion patterns between pregnancy and pseudopregnancy and the potential application of fecal corticoid metabolite monitoring for evaluating responses to stressors associated with practices used in breeding management. (C) 2002 Wiley-Liss, Inc. C1 Toronto Zoo, Scarborough, ON M1B 5K7, Canada. Univ Guelph, Ontario Vet Coll, Dept Biomed Sci, Guelph, ON N1G 2W1, Canada. Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA USA. RP Goodrowe, KL (reprint author), Toronto Zoo, 361A Old Finch Ave, Scarborough, ON M1B 5K7, Canada. NR 72 TC 28 Z9 31 U1 2 U2 16 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PY 2001 VL 20 IS 6 BP 517 EP 536 DI 10.1002/zoo.10001 PG 20 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 532WD UT WOS:000174497300005 ER PT J AU Ahyong, ST Manning, RB Reed, K AF Ahyong, ST Manning, RB Reed, K TI Revision of Pseudosquillana Cappola & Manning, 1995 (Crustacea : Stomatopoda : Pseudosquillidae) SO RAFFLES BULLETIN OF ZOOLOGY LA English DT Article DE Pseudosquillana; Pseudosquillidae; Stomatopoda; taxonomy ID CRUSTACEA AB Pseudosquillana Cappola & Manning, 1995, was recognized for Pseudosquilla megalophthalma Bigelow, 1893, and its presumed synonym, P. richeri Moosa, 1991. Restudy of types and other material of P. megalophthalma and P. richeri revealed both species to be distinct; P. richeri is removed from synonymy. The generic definition of Pseudosquillana, previously based on diagnostic characters of both species, is redefined and an amended key to the genera of the Pseudosquillidae is given. Both species have wide Indo-West Pacific distributions, but most records of Pseudosquillana megalophthalma are based on P. richeri. Pseudosquillana richeri is known from the western Indian Ocean, eastwards to Indonesia, New Caledonia and now Australia, Japan, and French Polynesia. Pseudosquillana megalophthalma is known from the type locality, Mauritius, and now from New Caledonia. The ectoparasitic gastropod, Caledoniella montrouzieri Souverbie is reported from P. richeri and constitutes the first record for a member of the Pseudosquillidae. C1 Dept Marine Invertebrates, Sydney, NSW 2010, Australia. Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Ahyong, ST (reprint author), Dept Marine Invertebrates, Australian Museum 6 Coll St, Sydney, NSW 2010, Australia. NR 35 TC 1 Z9 1 U1 0 U2 0 PU NATL UNIV SINGAPORE, SCHOOL BIOLOGICAL SCIENCES PI SINGAPORE PA DEPT ZOOLOGY, KENT RIDGE, SINGAPORE 0511, SINGAPORE SN 0217-2445 J9 RAFFLES B ZOOL JI Raffles Bull. Zool. PD DEC 31 PY 2000 VL 48 IS 2 BP 301 EP 311 PG 11 WC Zoology SC Zoology GA 392YZ UT WOS:000166441500014 ER PT J AU Russell, SS MacPherson, GJ Leshin, LA McKeegan, KD AF Russell, SS MacPherson, GJ Leshin, LA McKeegan, KD TI O-16 enrichments in aluminum-rich chondrules from ordinary chondrites SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE O-16; chondrules; ordinary chondrites; calcium-aluminium inclusions; isotopes ID OXYGEN ISOTOPIC ANOMALIES; CARBONACEOUS CHONDRITES; SOLAR NEBULA; INCLUSIONS; ALLENDE; OLIVINE; METEORITES; DIFFUSION; AL-26 AB The oxygen isotopic compositions of seven Al-rich chondrules from four unequilibrated ordinary chondrites were measured in situ using an ion microprobe. On an oxygen three isotope plot, the data are continuous with the ordinary chondrite ferromagnesian chondrule field but extend it to more O-16-enriched values along a mixing line of slope = 0.83 +/- 0.09, with the lightest value recorded at delta O-18 = -15.7 +/- 1.8 parts per thousand and delta O-17 = -13.5 +/- 2.6 parts per thousand. If Al-rich chondrules were mixtures of ferromagnesian chondrules and CAI material, their bulk chemical compositions would require them to exhibit larger O-16 enrichments than we observe. Therefore, Al-rich chondrules are not simple mixtures of these two components. Three chondrules exhibit significant internal isotopic heterogeneity indicative of partial exchange with a gaseous reservoir. Porphyritic Al-rich chondrules are consistently O-16-rich relative to nonporphyritic ones, suggesting that degree of melting is a key factor and pointing to a nebular setting for the isotopic exchange process. Because Al-rich chondrules are closely related to ferromagnesian chondrules, their radiogenic Mg isotopic abundances can plausibly be applied to help constrain the timing or location of chondrule formation. (C) 2000 Elsevier Science B.V. All rights reserved. C1 Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20560 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Russell, SS (reprint author), Nat Hist Museum, Dept Mineral, Cromwell Rd, London SW7 5BD, England. RI McKeegan, Kevin/A-4107-2008; UCLA, SIMS/A-1459-2011 OI McKeegan, Kevin/0000-0002-1827-729X; NR 44 TC 41 Z9 44 U1 2 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD DEC 30 PY 2000 VL 184 IS 1 BP 57 EP 74 DI 10.1016/S0012-821X(00)00309-5 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 391CA UT WOS:000166335500005 ER PT J AU Ramachandran, B Balakrishnan, N Dalgarno, A AF Ramachandran, B Balakrishnan, N Dalgarno, A TI Vibrational-rotational distributions of NO formed from N+O-2 reactive collisions SO CHEMICAL PHYSICS LETTERS LA English DT Article ID POTENTIAL-ENERGY SURFACE; NITRIC-OXIDE; ATMOSPHERIC REACTION; RATE CONSTANTS; EXCITATION; DYNAMICS; (2)A'; THERMOSPHERE; NITROGEN; ATOMS AB We present the results of quasi-classical trajectory (QCT) calculations for the N(S-4) + O-2 reaction over a broad range of collision energies with scaled ab initio potential energy surfaces of the (2)A' and (4)A' electronic states. The analysis of product rovibrational distributions support the suggestion that this reaction is a source of highly excited NO in the upper atmosphere, The computed NO vibrational distribution is found to be in good agreement with a recent measurement. (C) 2000 Elsevier Science B.V. All rights reserved. C1 Louisiana Tech Univ, Ruston, LA 71272 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Ramachandran, B (reprint author), Louisiana Tech Univ, POB 10348, Ruston, LA 71272 USA. OI Ramachandran, Bala/0000-0002-5179-5750 NR 28 TC 12 Z9 12 U1 1 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD DEC 29 PY 2000 VL 332 IS 5-6 BP 562 EP 568 DI 10.1016/S0009-2614(00)01302-6 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 389JY UT WOS:000166235900022 ER PT J AU Lemaitre, R Bermudez, A AF Lemaitre, R Bermudez, A TI A new cyclodorippoid crab of the genus Cymonomoides Tavares, 1993 (Crustacea : Decapoda : Brachyura : Cymonomidae) from the Caribbean coast of Colombia SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new Cyclodorippoidea crab species, Cymonomoides fitoi, of the family Cymonomidae Bouvier, is described and illustrated based on specimens collected from the upper slope region off the Caribbean coast of Colombia. This new species is the fourth known in the genus Cymonomoides Tavares, and the third from the western Atlantic. This new species is compared to its congeners, from which it is distinguished by features of the ocular peduncles, dorsal surface of the carapace, and spination on the dactyls of fourth and fifth pereopods. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. Univ Nacl Colombia, Inst Invest Marinas & Costeras, Santa Marta, Colombia. RP Lemaitre, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. NR 9 TC 4 Z9 6 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 29 PY 2000 VL 113 IS 4 BP 974 EP 979 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 389YA UT WOS:000166265200013 ER PT J AU Schotte, M AF Schotte, M TI Thermosphaeroma mendozai, a new species from hot springs in northern Chihuahua, Mexico (Crustacea : Isopoda : Sphaeromatidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new species of Thermosphaeroma (T. mendozai) is described from a collection of specimens found in hot springs in Chihuahua State, Mexico. Apomorphic characters are seen in the frontal lamina, pleotelson, and uropods. A new record is given for T. subequalum and the morphology of the female brood pouch is described for T. smithi., Bowman's (1981) key to species of Thermosphaeroma is amended to include all known congeners. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Schotte, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. NR 7 TC 5 Z9 5 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 29 PY 2000 VL 113 IS 4 BP 989 EP 995 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 389YA UT WOS:000166265200015 ER PT J AU Ferrari, FD Markhaseva, EL AF Ferrari, FD Markhaseva, EL TI Brachycalanus flemingeri and B-brodskyi, two new copepods (Crustacea : Calanoida : Phaennidae) from benthopelagic waters of the tropical Pacific SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID ANTARCTIC OCEAN; REDESCRIPTION; BELIZE; GENUS AB Brachycalanus flemingeri, new species, has three setae on coral endite of maxilla 1, a bifurcate worm-like sensory seta on the exopod of maxilla 2, a distal, semicircular protrusion posteriorly on the basis of swimming leg 1, and lacks a medial seta on coxa of swimming leg 4. Brachycalumus brodskyi, new species, is differentiated by its large size, 4.0 mm, and a semi circular row of small denticles distally and posteriorly on the basis of swimming leg 1. Brachycalanus ordinarius (Grice, 1972) is redescribed and separated from the remaining species by the exopod of maxilla 2 with a distally constricted worm-like seta with a small lobe near the point of constriction. All three species have nine sensory setae on the distal basal lobe plus exopod of maxilla 2; this number of sensory setae has been reported for one other phaennid copepod and several scolecitrichids. Suggested shared derived character states for the species of Brachycalanus Farran, 1905 are epicuticular extensions of the female genital complex and the following two abdominal somites, and knife-like aesthetascs on female antenna 1. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. RP Ferrari, FD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. NR 21 TC 16 Z9 20 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 29 PY 2000 VL 113 IS 4 BP 1064 EP 1078 PG 15 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 389YA UT WOS:000166265200018 ER PT J AU Ferrari, FD Markhaseva, EL AF Ferrari, FD Markhaseva, EL TI Grievella shanki, a new genus and species of scolecitrichid calanoid copepod (Crustacea) from a hydrothermal vent along the southern East Pacific Rise SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID OCEAN AB Four derived states separate the calanoid copepod Grievella shanki, new genus and species, from other scolecitrichids: small integumental bumps on the genital complex; an ear-like extension on articulating segment 22 of antenna 1; two lateral setae on the distal exopodal segment of swimming leg 2; a denticle-like attenuation of the proximal praecoxal lobe of maxilla 2, The first probably is an autapomorphy for the species; the second, third and fourth are presumed synapomorphies for species of the new genus. The last derived state is convergent with some species of the calanoid superfamilies Epacteriscoidea, Centropagoidea and Megacalanoidea, but it is a synapomorphy within the Clausocalanoidea to which Grievella shanki belongs. Five setae on the proximal praecoxal lobe of maxilla 2 and three setae on the distal praecoxal lobe of the maxilliped separate Grievella shanki from species of Diaixidae, Parkiidae and Tharybidae, and species of Phaennidae, respectively. The states of these characters for Grievella shanki may be plesiomorphic to the states expressed in Diaixidae, Parkiidae, Tharybidae and Phaennidae so assignment of this species to the Scolecitrichidae is tentative. The number and kind of sensory setae on the distal basal lobe plus exopod of maxilla 2 alone are not adequate to diagnose the Scolecitrichidae, or to separate all of its species from those of the other families with these sensory setae. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool MRC 534, Washington, DC 20560 USA. Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. RP Ferrari, FD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool MRC 534, Washington, DC 20560 USA. NR 13 TC 18 Z9 24 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD DEC 29 PY 2000 VL 113 IS 4 BP 1079 EP 1088 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 389YA UT WOS:000166265200019 ER PT J AU Carilli, CL Menten, KM Stocke, JT Perlman, E Vermeulen, R Briggs, F de Bruyn, AG Conway, J Moore, CP AF Carilli, CL Menten, KM Stocke, JT Perlman, E Vermeulen, R Briggs, F de Bruyn, AG Conway, J Moore, CP TI Astronomical constraints on the cosmic evolution of the fine structure constant and possible quantum dimensions SO PHYSICAL REVIEW LETTERS LA English DT Article ID TIME-VARIATION; FUNDAMENTAL CONSTANTS; PHYSICAL CONSTANTS; LIMITS; NUCLEOSYNTHESIS; PKS-1413+135; ABSORPTION AB We present measurements of absorption by the 21 cm hyperfine transition of neutral hydrogen toward radio sources at substantial look-back times. These data are used in combination with observations of rotational transitions of common interstellar molecules to set limits on the evolution of the fine structure constant: (alpha) over dot/alpha < 3.5 X 10-(15) yr(-1), to a look-back time of 4.8 Gyr. In the context of string theory, the limit on the secular evolution of the scale factor of the compact dimensions, R, is (R) over dot/R < 10(-15) yr(-1) Including terrestrial and other astronomical measurements places a limits on slow oscillations of R from the present to the epoch of cosmic nucleosynthesis, just seconds after the big bang, of DeltaR/R < 10(-15). C1 Natl Radio Astron Observ, Socorro, NM 87801 USA. Max Planck Inst Radioastron, D-53121 Bonn, Germany. Univ Colorado, Boulder, CO 80309 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Netherlands Fdn Res Astron, NL-7990 AA Dwingeloo, Netherlands. Univ Groningen, Kapteyn Res Inst, Groningen, Netherlands. Onsala Space Observ, S-43900 Onsala, Sweden. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Carilli, CL (reprint author), Natl Radio Astron Observ, Socorro, NM 87801 USA. NR 34 TC 53 Z9 53 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 25 PY 2000 VL 85 IS 26 BP 5511 EP 5514 DI 10.1103/PhysRevLett.85.5511 PN 1 PG 4 WC Physics, Multidisciplinary SC Physics GA 387QD UT WOS:000166132500008 PM 11136034 ER PT J AU Fernandez, L Vari, RP AF Fernandez, L Vari, RP TI New species of Trichomycterus (Teleostei : Siluriformes : Trichomycteridae) lacking a pelvic fin and girdle from the Andes of Argentina SO COPEIA LA English DT Article AB Trichomycterus catamarcensis, new species, is described hem a tributary to the high elevation Laguna Blanca in Departamento Belen, Provincia de Catamarca, Argentina, Characters from various body systems indicate that the new species is a member of the subfamily Trichomycterinae. The new species is separable from the other members of the Trichomycterinae by its lack of the pelvic fins and girdle, the form of the body and caudal fin, the number of dorsal fin rays and ribs, its pigmentation pattern, the form of premaxillary dentition, and the maximum body size. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. Consejo Nacl Invest Cient & Tecn, Fdn Miguel Lillo, RA-4000 San Miguel De Tucuman, Tucuman, Argentina. RP Vari, RP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM vari.richard@nmnh.si.edu NR 26 TC 27 Z9 29 U1 0 U2 0 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD DEC 22 PY 2000 IS 4 BP 990 EP 996 DI 10.1643/0045-8511(2000)000[0990:NSOTTS]2.0.CO;2 PG 7 WC Zoology SC Zoology GA 390DY UT WOS:000166281500008 ER PT J AU Omland, KE Tarr, CL Boarman, WI Marzluff, JM Fleischer, RC AF Omland, KE Tarr, CL Boarman, WI Marzluff, JM Fleischer, RC TI Cryptic genetic variation and paraphyly in ravens SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE paraphyletic species; speciation; phylogeography; mitochondrial DNA; microsatellites; Corvus corax ID MITOCHONDRIAL-DNA VARIATION; NORTH-AMERICAN CHICKADEES; CONTROL-REGION SEQUENCES; EVOLUTIONARY RELATIONSHIPS; MOLECULAR PHYLOGENY; CORVUS-KUBARYI; MARIANA CROW; SPECIATION; PRIMERS; DIVERSIFICATION AB Widespread species that are morphologically uniform may be likely to harbour cryptic genetic variation. Common ravens (Corvus corax) have an extensive range covering nearly the entire Northern Hemisphere, but show little discrete phenotypic variation. We obtained tissue samples from throughout much of this range and collected mitochondrial sequence and nuclear microsatellite data. Our study revealed a deep genetic break between ravens from the western United States and ravens from throughout the rest of the world. These two groups, the 'California clads' and the 'Holarctic clade' are well supported and over 4% divergent in mitochondrial coding sequence. Microsatellites also reveal significant differentiation between these two groups. Ravens from;Minnesota, Maine and Alaska are more similar to ravens from Asia and Europe than they are to ravens from California. The two clades come in contact over a huge area of the western United States, with mixtures of the two mitochondrial groups present in Washington, Idaho and California. In addition, the restricted range Chihuahuan raven (Corvus cryptoleucus) of the south-west United States and Mexico is genetically nested within the paraphyletic common raven. Our findings suggest that the common raven may have formerly consisted of two allopatric groups that may be in the process of remerging. C1 Smithsonian Inst, Natl Zool Pk, Mol Genet Lab, Washington, DC 20008 USA. Penn State Univ, Dept Biol, University Pk, PA 16802 USA. Univ Calif Riverside, Dept Biol, US Geol Survey, Riverside, CA 92521 USA. Univ Washington, Coll Forest Resources, Seattle, WA 98195 USA. RP Omland, KE (reprint author), Univ Maryland Baltimore Cty, Dept Biol Sci, 1000 Hilltop Circle, Baltimore, MD 21250 USA. EM omland@umbc.edu RI Omland, Kevin/A-8887-2010 OI Omland, Kevin/0000-0002-3863-5509 NR 60 TC 80 Z9 84 U1 2 U2 14 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD DEC 22 PY 2000 VL 267 IS 1461 BP 2475 EP 2482 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 392RT UT WOS:000166426100002 PM 11197122 ER PT J AU Croft, RAC Metzler, CA AF Croft, RAC Metzler, CA TI Weak-lensing surveys and the intrinsic correlation of galaxy ellipticities SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; gravitational lensing; large-scale structure of universe ID COLD DARK-MATTER; LARGE-SCALE STRUCTURE; PISCES-PERSEUS SUPERCLUSTER; ANGULAR-MOMENTUM; TIDAL TORQUES; NONLINEAR EVOLUTION; INITIAL CONDITIONS; ABELL CLUSTERS; POWER SPECTRUM; RICH CLUSTERS AB We explore the possibility that an intrinsic correlation between galaxy ellipticities arising during the galaxy formation process may account for part of the shear signal recently reported by several groups engaged in weak gravitational lensing surveys. Using high-resolution N-body simulations, we measure the projected ellipticities of dark matter halos and their correlations as a function of pair separation. With this simplifying, but not necessarily realistic, assumption (halo shapes as a proxy for galaxy shapes), we find a positive detection of correlations up to scales of at least 20 h(-1) Mpc (limited by the box size). The signal is not strongly affected by variations in the halo-finding technique, or by the resolution of the simulations (over the range tested). We translate our three-dimensional results into angular measurements of ellipticity correlation functions and shear variance, which can be directly compared to observational results. We also make simulated angular surveys by projecting our simulation boxes onto the plane of the sky and applying a radial selection function. Measurements from these catalogs are consistent with the analytic projection of the statistics. Interestingly, the shear variance we measure is a small, but not entirely negligible, fraction (from similar to 10%-20%, depending on the angular scale) of that seen by the observational groups, and the ellipticity correlation functions approximately mimic the functional form expected to be caused by weak lensing. The amplitude of these projected quantities depends strongly on the width in redshift of the galaxy distribution. If in the future photometric redshifts are used to pick out a screen of background galaxies with a small redshift width, then the intrinsic correlation may become comparable to the weak-lensing signal. Although we are dealing with simulated dark matter halos, we might expect there to be a similar sort of signal when real galaxies are used. This could be checked fruitfully using a nearby sample with known redshifts. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Croft, RAC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Croft, Rupert/N-8707-2014 OI Croft, Rupert/0000-0003-0697-2583 NR 57 TC 145 Z9 146 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2000 VL 545 IS 2 BP 561 EP 571 DI 10.1086/317856 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 385UW UT WOS:000166023400002 ER PT J AU Cohen, AS Hewitt, JN Moore, CB Haarsma, DB AF Cohen, AS Hewitt, JN Moore, CB Haarsma, DB TI Further investigation of the time delay, magnification ratios, and variability in the gravitational lens 0218+357 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (0218+357); distance scale; gravitational lensing; radio continuum : galaxies ID SMALLEST EINSTEIN RING; SYSTEM B0218+357; HUBBLE-CONSTANT; GALAXY NGC4258; LIGHT; RADIO; LENS-0957+561; QSO-0957+561; ABSORPTION; Q0957+561 AB High-precision VLA flux density measurements for the lensed images of 0218+357 yield a time delay of 10.1(-1.6)(+1.5) days (95% confidence). This is consistent with independent measurements carried out at the same epoch by Biggs and colleagues in 1999, lending confidence to the robustness of the time delay measurement. However, since both measurements make use of the same features in the light curves, it is possible that the effects of unmodeled processes, such as scintillation or microlensing, are biasing both time delay measurements in the same way. Our time delay estimates result in confidence intervals that are somewhat larger than those of Biggs et al., probably because we adopt a more general model of the source variability, allowing for constant and variable components. When considered in relation to the lens mass model of Biggs et al., our best-fit time delay implies a Hubble constant of H-0 = 71(-23)(+17) km s(-1) Mpc(-1) for Omega (0) = 1 and lambda (0) = (95% confidence; filled beam). This confidence interval for H-0 does not reflect systematic error, which may be substantial, as a result of uncertainty in the position of the lens galaxy. We also measure the flux ratio of the variable components of 0218+357, a measurement of a small region that should more closely represent the true lens magnification ratio. We find ratios of 3.2(-0.4)(+0.3) (95% confidence; 8 GHz) and 4.3(-0.8)(+0.5) (15 GHz). Unlike the reported flux ratios on scales of 0 " .1, these ratios are not significantly different. We investigate the significance of apparent differences in the variability properties of the two images of the background active galactic nucleus. We conclude that the differences are not significant and that time series much longer than our 100 day time series will be required to investigate propagation effects in this way. C1 MIT, Dept Phys, Cambridge, MA 02139 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. Calvin Coll, Dept Phys & Astron, Grand Rapids, MI 49546 USA. RP Cohen, AS (reprint author), MIT, Dept Phys, Room 37-607, Cambridge, MA 02139 USA. NR 50 TC 36 Z9 36 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2000 VL 545 IS 2 BP 578 EP 590 DI 10.1086/317830 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 385UW UT WOS:000166023400004 ER PT J AU Monnier, JD Tuthill, PG Danchi, WC AF Monnier, JD Tuthill, PG Danchi, WC TI Diffraction-limited near-IR imaging at Keck reveals asymmetric, time-variable nebula around carbon star CIT 6 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars : AGB and post-AGB; stars : winds, outflows; techniques : interferometric ID INFRARED STARS; WAVELENGTH DEPENDENCE; INTERFEROMETRY; TELESCOPE; OBJECTS; POLARIZATION; PHOTOMETRY; IRC+10216; MICRONS; PHASE AB We present multiepoch, diffraction-limited images of the nebula around the carbon star CIT 6 at 2.2 and 3.1 mum from aperture masking on the Keck I Telescope. The near-IR nebula is resolved into two main components, an elongated, bright feature showing time-variable asymmetry and a fainter component about 60 mas away with a cooler color temperature. These images were precisely registered (similar to 35 mas) with respect to recent visible images from the Hubble Space Telescope (Trammell et al.), which showed a bipolar structure in scattered light. The dominant near-IR feature is associated with the northern lobe of this scattering nebula, and the multiwavelength data set can be understood in terms of a bipolar dust shell around CIT 6. Variability of the near-IR morphology is qualitatively consistent with previously observed changes in red polarization, caused by varying illumination geometry due to nonuniform dust production. The blue emission morphology and polarization properties cannot be explained by the above model alone, but require the presence of a wide binary companion in the vicinity of the southern polar lobe. The physical mechanisms responsible for the breaking of spherical symmetry around extreme carbon stars, such as CIT 6 and IRC +10216, remain uncertain. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Sydney, Sch Phys, Chatterton Astron Dept, Sydney, NSW 2006, Australia. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Smithsonian Astrophys Observ, MS 42,60 Garden St, Cambridge, MA 02138 USA. EM jmonnier@cfa.harvard.edu; gekko@physics.usyd.edu.au; wcd@ssl.berkeley.edu NR 34 TC 35 Z9 35 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2000 VL 545 IS 2 BP 957 EP 964 DI 10.1086/317857 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 385UW UT WOS:000166023400035 ER PT J AU Drake, JJ Peres, G Orlando, S Laming, JM Maggio, A AF Drake, JJ Peres, G Orlando, S Laming, JM Maggio, A TI On stellar coronae and solar active regions SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars : coronae; stars : individual (epsilon Eridani, xi Bootis); Sun : corona; Sun : X-rays, gamma rays; X-rays : stars ID EXTREME-ULTRAVIOLET SPECTRUM; DWARF EPSILON-ERIDANI; MAIN-SEQUENCE STARS; X-RAY-EMISSION; K-TYPE STARS; LINE EMISSION; COOL STARS; BOOTIS-A; F-TYPE; ABUNDANCES AB Based on Yohkoh Soft X-Ray Telescope (SXT) observations of the Sun near peak activity level obtained on 1992 January 6, we search for coronal structures that have emission measure distributions EM(T) that match the observed stellar coronal emission measure distributions derived for the intermediate-activity stars epsilon Eri (K2 V) and xi Boo A (G8 V) from Extreme Ultraviolet Explorer spectroscopic observations. We find that the temperatures of the peaks of the observed stellar distributions EM(T), as well as their slopes in the temperature range are very similar to those 6.0 less than or similar to log T less than or similar to 6.5, obtained for the brightest of the solar active regions in the 1992 January 6 SXT images. The observed slopes correspond approximately to EM proportional to T-beta with beta similar to 4, which is much steeper than predicted by static, uniformly heated loop models. Plasma densities in the coronae of epsilon Eri and xi Boo A are also observed to be essentially the same as the plasma densities typical of solar active regions. These data provide the best observational support yet obtained for the hypothesis that solar-like stars up to the activity levels of epsilon Eri (K2 V) and xi Boo A are dominated by active regions similar to, though possibly considerably larger than, those observed on the Sun. The surface filling factor of bright active regions needed to explain the observed stellar emission measures is approximately unity. We speculate on the scenario in which small-scale "nanoflares" II dominate the heating of active regions up to activity levels similar to those of epsilon Eri (K2 V) and xi Boo A. At higher activity levels still, the interactions of the active regions themselves may lead to increasing flaring on larger scales that is responsible for heating plasma to the observed coronal temperatures of T greater than or similar to 10(7) K on very active stars. Observations of X-ray and EUV light curves using more sensitive instruments than are currently available, together with determinations of plasma densities over the full range of coronal temperatures (10(6)-10(7) K and higher), will be important to confirm flare heating hypotheses and to elicit further details concerning coronal structures at solar-like active region temperatures (T less than or similar to 5 x 10(6) K)and the temperatures that characterize the most active stars (T greater than or similar to 10(7) K). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Palermo, Dipartimento Sci Fisiche & Astron, Sez Astron, I-90134 Palermo, Italy. European Space Agcy, Dept Space Sci, ESTEC SO, Solar Syst Div, NL-2200 AG Noordwijk, Netherlands. SFA Inc, Landover, MD 20785 USA. USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. Osservatorio Astron, I-90134 Palermo, Italy. RP Harvard Smithsonian Ctr Astrophys, MS-70,60 Garden St, Cambridge, MA 02138 USA. RI Maggio, Antonio/P-5700-2015; OI Maggio, Antonio/0000-0001-5154-6108; Orlando, Salvatore/0000-0003-2836-540X NR 59 TC 75 Z9 75 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2000 VL 545 IS 2 BP 1074 EP 1083 DI 10.1086/317820 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 385UW UT WOS:000166023400048 ER PT J AU Laming, JM Kink, I Takacs, E Porto, JV Gillaspy, JD Silver, EH Schnopper, HW Bandler, SR Brickhouse, NS Murray, SS Barbera, M Bhatia, AK Doschek, GA Madden, N Landis, D Beeman, J Haller, EE AF Laming, JM Kink, I Takacs, E Porto, JV Gillaspy, JD Silver, EH Schnopper, HW Bandler, SR Brickhouse, NS Murray, SS Barbera, M Bhatia, AK Doschek, GA Madden, N Landis, D Beeman, J Haller, EE TI Emission-line intensity ratios in Fe XVII observed with a microcalorimeter on an electron beam ion trap SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; methods : laboratory; stars : individual (Capella); Sun : corona; techniques : spectroscopic; X-rays : general ID X-RAY-SPECTRA; SOLAR-FLARE; ACTIVE-REGION; POLARIZATION; PLASMAS; DENSITY AB We report new observations of emission line intensity ratios of Fe XVII under controlled experimental conditions, using the National Institute of Standards and Technology electron beam ion trap (EBIT) with a microcalorimeter detector. We compare our observations with collisional-radiative models using atomic data computed in distorted wave and R-matrix approximations, which follow the transfer of the polarization of level populations through radiative cascades. Our results for the intensity ratio of the 2p(6) S-1(0)-2p(5)3d P-1(1) 15.014 Angstrom line to the 2p(6) S-1(0)- 2p(5) 3d D-3(1) 15.265 Angstrom line are 2.94 +/- 0.18 and 2.50 +/- 0.13 at beam energies of 900 and 1250 eV, respectively. These results are not consistent with collisional-radiative models and support conclusions from earlier EBIT work at the Lawrence Livermore National Laboratory that the degree of resonance scattering in the solar 15.014 Angstrom line has been overestimated in previous analyses. Further observations assess the intensity ratio of the three lines between the 2p(6)-2p(5)3s configurations to the three lines between the 2p(6)-2p(5)3d configurations. Both R-matrix and distorted wave approximations agree with each other and our experimental results much better than most solar and stellar observations, suggesting that other processes not present in our experiment must play a role in forming the Fe XVII spectrum in solar and astrophysical plasmas. C1 USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. MIT, Cambridge, MA 02139 USA. Univ Debrecen, H-4026 Debrecen, Hungary. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron GS Vaiana, I-90134 Palermo, Italy. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. RP Laming, JM (reprint author), USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA. RI Bandler, Simon/A-6258-2010; OI Bandler, Simon/0000-0002-5112-8106; Brickhouse, Nancy/0000-0002-8704-4473 NR 31 TC 71 Z9 72 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2000 VL 545 IS 2 BP L161 EP L164 DI 10.1086/317876 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393EL UT WOS:000166456200021 ER PT J AU Matsushita, S Kawabe, R Matsumoto, H Tsuru, TG Kohno, K Morita, KI Okumura, SK Vila-Vilaro, B AF Matsushita, S Kawabe, R Matsumoto, H Tsuru, TG Kohno, K Morita, KI Okumura, SK Vila-Vilaro, B TI Formation of a massive black hole at the center of the superbubble in M82 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies : individual (M82, NGC 3034); galaxies : ISM; galaxies : starburst; ISM : bubbles ID STARBURST GALAXY M82; NUCLEUS; M-82; GAS AB We performed (CO)-C-12 (1-0), (CO)-C-13 (1-0), and HCN (1-0) interferometric observations of the central region (about 450 pc in radius) of M82 with the Nobeyama Millimeter Array and have successfully imaged a molecular superbubble and spurs. The center of the superbubble is clearly shifted from the nucleus by 140 pc. This position is close to that of the massive black hole (BH) of greater than or similar to 460 M. and the 2.2 mum secondary peak (a luminous, supergiant-dominated cluster), which strongly suggests that these objects may be related to the formation of the superbubble. Consideration of star formation in the cluster based on the infrared data indicates that (1) the energy release from supernovae can account for the kinetic energy of the superbubble, (2) the total mass of stellar-mass BHs available for building up the massive BH may be much higher than 460 M., and (3) it is possible to form, the middle-mass BH of 10(2)-10(3) M. within the timescale of the superbubble. We suggest that the massive BH was produced and is growing in the intense starburst region. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Submillimeter Array, Hilo, HI 96721 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Kyoto Univ, Fac Sci, Dept Phys, Kyoto 6068502, Japan. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Matsushita, S (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Submillimeter Array, POB 824, Hilo, HI 96721 USA. NR 35 TC 39 Z9 41 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2000 VL 545 IS 2 BP L107 EP L111 DI 10.1086/317880 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393EL UT WOS:000166456200009 ER PT J AU Muzerolle, J Briceno, C Calvet, N Hartmann, L Hillenbrand, L Gullbring, E AF Muzerolle, J Briceno, C Calvet, N Hartmann, L Hillenbrand, L Gullbring, E TI Detection of disk accretion at the substellar limit SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars : formation; stars : individual (V410 Anon 13) stars : low-mass, brown dwarfs; stars : pre-main-sequence; techniques : spectroscopic ID T-TAURI STARS; MAGNETOSPHERIC ACCRETION; YOUNG OBJECTS; IRRADIATION; EMISSION AB We have made the first definitive detection of disk accretion in an object near or below the substellar limit. We obtained an echelle-resolution spectrum of the very low mass T Tauri star V410 Anon 13; the emission-line profile of H alpha clearly exhibits the large line width and asymmetry characteristic of a free-falling accretion flow. We use magnetospheric accretion models of the line profile to estimate the mass accretion rate in this object, which is the smallest yet determined. We further augment this with models of the accretion shock and disk to explain the absence of both optical veiling and an infrared excess, obtaining a firm upper limit to the accretion rate that is consistent with the H alpha model. Our results indicate that disk accretion via magnetospheric infall occurs even in the lowest mass young objects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ctr Invest Astron, Merida 5101A, Venezuela. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Stockholm Observ, S-13336 Saltsjobaden, Sweden. RP Muzerolle, J (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. NR 24 TC 56 Z9 56 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2000 VL 545 IS 2 BP L141 EP L144 DI 10.1086/317877 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 393EL UT WOS:000166456200016 ER PT J AU Schultz, TR AF Schultz, TR TI In search of ant ancestors SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Editorial Material ID EARLY EVOLUTION; HYMENOPTERA; FORMICIDAE; AMBER C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 188, Washington, DC 20560 USA. RP Schultz, TR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 188, Washington, DC 20560 USA. EM schultz@onyx.si.edu NR 31 TC 29 Z9 34 U1 1 U2 10 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD DEC 19 PY 2000 VL 97 IS 26 BP 14028 EP 14029 DI 10.1073/pnas.011513798 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 385FV UT WOS:000165993700005 PM 11106367 ER PT J AU Guan, YB McKeegan, KD MacPherson, GJ AF Guan, YB McKeegan, KD MacPherson, GJ TI Oxygen isotopes in calcium-aluminum-rich inclusions from enstatite chondrites: new evidence for a single CAI source in the solar nebula (vol 181, pg 271, 2000) SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Correction C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP MacPherson, GJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD DEC 15 PY 2000 VL 183 IS 3-4 BP 557 EP 558 DI 10.1016/S0012-821X(00)00293-4 PG 2 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 385XH UT WOS:000166030100019 ER PT J AU Sewall, JO Sloan, LC Huber, M Wing, S AF Sewall, JO Sloan, LC Huber, M Wing, S TI Climate sensitivity to changes in land surface characteristics SO GLOBAL AND PLANETARY CHANGE LA English DT Article DE Cenozoic; paleoclimate; climate modeling; land surface; North America ID GENERAL-CIRCULATION MODELS; GLOBAL CLIMATE; STOMATAL-RESISTANCE; CENOZOIC TECTONICS; SOUTH-AMERICA; CENTRAL ANDES; EVOLUTION; PLATEAU; EOCENE; PALEOCLIMATES AB Using a recently developed global vegetation distribution, topography, and shorelines for the Early Eocene in conjunction with the Genesis version 2.0 climate model, we investigate the influences that these new boundary conditions have on global climate. Global mean climate changes little in response to the subtle changes we made; differences in mean annual and seasonal surface temperatures over northern and southern hemispheric land, respectively, are on the order of 0.5 degreesC. In contrast, and perhaps more importantly, continental scale climate exhibits significant responses. Increased peak elevations and topographic detail result in larger amplitude planetary similar to4 mm/day and decreases by 7-9 mm/day in the proto Himalayan region. Surface temperatures change by up to 18 degreesC as a direct result of elevation modifications. Increased leaf area index (LAI), as a result of altered vegetation distributions, reduces temperatures by up to 6 degreesC. Decreasing the size of the Mississippi embayment decreases inland precipitation by 1-2 mm/day. These climate responses to increased accuracy in boundary conditions indicate that "improved" boundary conditions may play an important role in producing modeled paleoclimates that approach the proxy data more closely. (C) 2000 Elsevier Science B.V. All rights reserved. C1 Univ Calif Santa Cruz, Dept Earth Sci, Santa Cruz, CA 95064 USA. Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Sewall, JO (reprint author), Univ Calif Santa Cruz, Dept Earth Sci, Santa Cruz, CA 95064 USA. RI Huber, Matthew/A-7677-2008; OI Huber, Matthew/0000-0002-2771-9977; Wing, Scott/0000-0002-2954-8905 NR 45 TC 70 Z9 72 U1 2 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-8181 J9 GLOBAL PLANET CHANGE JI Glob. Planet. Change PD DEC 15 PY 2000 VL 26 IS 4 BP 445 EP 465 DI 10.1016/S0921-8181(00)00056-4 PG 21 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 385WJ UT WOS:000166027900007 ER PT J AU Petit, RE Harasewych, MG AF Petit, RE Harasewych, MG TI Three new species of the genus Merica (Neogastropoda : Cancellariidae) from South Africa and the Philippines SO NAUTILUS LA English DT Article DE gastropoda; caenogastropoda; recent; western Pacific AB Three new species of the cancellariid genus Merica are described: Merica lussii from South Africa, and M, deynzeri and M. ektyphos from the southern Philippines. The South African Merica lussii has previously been misidentified in the literature as Cancellaria bifasciata Deshayes, 1830, a junior subjective synonym of C. oblonga Sowerby, 1825, from which it differs in having a broader, stepped spire, a proportionally shorter but broader aperture, and a deeply impressed sutural canal. Merica deynzeri differs from other Philippine species of Merica by its deeply impressed sutural canal, its much stronger and coarser axial and spiral sculpture, more rounded aperture, and its lack of banding pattern. Merica ektyphos can be distinguished from all other described species of Merica in its distinctively heavy inflated shell, as well as by its extremely coarse axial and spiral sculpture. C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Petit, RE (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20560 USA. NR 42 TC 3 Z9 3 U1 0 U2 0 PU BAILEY-MATTHEWS SHELL MUSEUM PI SANIBEL PA C/O DR JOSE H LEAL, ASSOCIATE/MANAGING EDITOR, 3075 SANIBEL-CAPTIVA RD, SANIBEL, FL 33957 USA SN 0028-1344 J9 NAUTILUS JI Nautilus PD DEC 15 PY 2000 VL 114 IS 4 BP 142 EP 148 PG 7 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 386GW UT WOS:000166053400002 ER PT J AU Pachucki, K Sapirstein, J AF Pachucki, K Sapirstein, J TI Contributions to helium fine structure of order m alpha(7) SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID HE-LIKE IONS; STRUCTURE SPLITTINGS; QED CORRECTIONS; STATES AB An effective Hamiltonian approach is used to analyst QED contributions to the fine structure of 2(3)P(J) levels in helium to order m alpha (7). Formulae for leading contributions are derived and their numerical values presented. C1 Univ Warsaw, Inst Theoret Phys, PL-00681 Warsaw, Poland. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. RP Pachucki, K (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. NR 15 TC 32 Z9 32 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD DEC 14 PY 2000 VL 33 IS 23 BP 5297 EP 5305 DI 10.1088/0953-4075/33/23/303 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 389WD UT WOS:000166260900003 ER PT J AU Esry, BD Sadeghpour, HR Wells, E Ben-Itzhak, I AF Esry, BD Sadeghpour, HR Wells, E Ben-Itzhak, I TI Charge exchange in slow H++D(1s) collisions SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID EARLY UNIVERSE; LOW ENERGIES; HD+; DEUTERIUM; CHEMISTRY; H+ AB We present the elastic and charge exchange cross sections for slow (meV) H+ + D(1s) collisions based upon a recently formulated adiabatic representation. This representation avoids many of the usual 'translational factor' issues, and those that remain have no significant effect for scattering in the n = 1 manifold. The cross sections are converged at the 1% level. The various Feshbach and shape resonances that form in the isotopic gap and in the charge transfer region are identified and compared with previous work. An exact analytical expression for the ratio of H+ + D(1s) and D+ +H(1s) charge exchange cross sections suitable for astrophysical simulations is presented. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Kansas State Univ, Dept Phys, JR Macdonald Lab, Manhattan, KS 66506 USA. RP Esry, BD (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. RI Ben-Itzhak, Itzik/J-8273-2012; Esry, Brett/H-7511-2013; OI Ben-Itzhak, Itzik/0000-0002-6214-3520; Esry, Brett/0000-0003-3207-8526; Wells, Eric/0000-0002-1044-4479 NR 22 TC 15 Z9 15 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD DEC 14 PY 2000 VL 33 IS 23 BP 5329 EP 5341 DI 10.1088/0953-4075/33/23/306 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 389WD UT WOS:000166260900006 ER PT J AU Bear, D Stoner, RE Walsworth, RL Kostelecky, VA Lane, CD AF Bear, D Stoner, RE Walsworth, RL Kostelecky, VA Lane, CD TI Limit on Lorentz and CPT violation of the neutron using a two-species noble-gas maser SO PHYSICAL REVIEW LETTERS LA English DT Article ID RADIATIVELY-INDUCED LORENTZ; HIGHER-DIMENSIONAL THEORIES; STANDARD MODEL; TESTING CPT; INVARIANCE; STRINGS; ELECTRODYNAMICS; CONSTRAINTS; ANISOTROPY; PARTICLES AB A search for sidereal variations in the frequency difference between co-located Xe-129 and He-3 Zeeman masers sets the most stringent limit to date on leading-order Lorentz and CPT violation involving the neutron, consistent with no effect at the level of 10(-31) GeV. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Indiana Univ, Dept Phys, Bloomington, IN 47405 USA. RP Bear, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Stoner, Richard/0000-0001-7949-6747 NR 50 TC 235 Z9 236 U1 2 U2 5 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 11 PY 2000 VL 85 IS 24 BP 5038 EP 5041 DI 10.1103/PhysRevLett.85.5038 PG 4 WC Physics, Multidisciplinary SC Physics GA 382CC UT WOS:000165800000007 ER PT J AU White, M Scott, D Pierpaoli, E AF White, M Scott, D Pierpaoli, E TI Boomerang returns unexpectedly SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : theory ID MICROWAVE BACKGROUND ANISOTROPIES; AMERICAN TEST FLIGHT; UNIVERSE; INFLATION; RADIATION; CONSTANT; POWER; OMEGA; FLAT AB Experimental study of the anisotropy in the cosmic microwave background (CMB) is gathering momentum. The eagerly awaited Boomerang results have lived up to expectations. They provide convincing evidence in favor of the standard paradigm: the universe is close to flat and with primordial fluctuations that are redolent of inflation. Further scrutiny reveals something even more exciting, however-two hints that there may be some unforeseen physical effects. First, the primary acoustic peak appears at slightly larger scales than expected. Although this may be explicable through a combination of mundane effects, we suggest that it is also prudent to consider the possibility that the universe might be marginally closed. The other hint is provided by a second peak, which appears less prominent than expected. This may indicate one of a number of possibilities, including increased damping length or tilted initial conditions, but also breaking of coherence or features in the initial power spectrum. Further data should test whether the current concordance model needs only to be tweaked, or to be enhanced in some fundamental way. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP White, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mwhite@cfa.harvard.edu; dscott@astro.ubc.ca; elena@astro.ubc.ca RI White, Martin/I-3880-2015; OI White, Martin/0000-0001-9912-5070; Pierpaoli, Elena/0000-0002-7957-8993 NR 39 TC 29 Z9 29 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2000 VL 545 IS 1 BP 1 EP 5 DI 10.1086/317817 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 385RW UT WOS:000166018300001 ER PT J AU Elvis, M AF Elvis, M TI A structure for quasars SO ASTROPHYSICAL JOURNAL LA English DT Review DE quasars : absorption lines; quasars : general ID ACTIVE GALACTIC NUCLEI; BROAD-ABSORPTION-LINE; X-RAY REFLECTION; C-IV ABSORPTION; EMISSION-LINE; SEYFERT-1 GALAXIES; COLD MATTER; BAL QSOS; STELLAR OBJECTS; ACCRETION DISK AB This paper proposes a simple, empirically derived, unifying structure for the inner regions of quasars. This structure is constructed to explain the broad absorption line regions (BALRs) and the narrow "associated" ultraviolet and X-ray "ionized" absorbers (NALs) and is also found to explain the broad emission line regions (BELRs) and several scattering features, including a substantial fraction of the broad X-ray Fe-K emission line and the biconical extended narrow emission line region (ENLR) structures seen on large kiloparsec scales in Seyfert images. The model proposes that a funnel-shaped thin shell outflow creates all of these features. The wind arises vertically from a narrow range of radii on a disk at BELR velocities. Radiation force then accelerates the flow radially, so that it bends outward to a cone angle of similar to 60 degrees and has a divergence angle of similar to6 degrees, to give a covering factor of similar to 10%. When the central continuum is viewed from the side, through this wind, narrow high-ionization "associated" ultraviolet absorption lines and the X-ray "ionized absorbers" are seen, as in many low-luminosity active galactic nuclei (AGNs). When viewed end-on, the full range of velocities is seen in absorption with a large total column density, giving rise to the broad absorption line systems seen in a minority of quasars, the BAL QSOs. The wind is both warm (similar to 10(6) K) and highly ionized. This warm highly ionized medium (WHIM) has a density of similar to 10(9) cm(-3), putting it in pressure equilibrium with the BELR clouds; the BELR is then a cool phase embedded in the overall outflow, avoiding cloud destruction through shear. The wind has the correct ionization parameter and filling factor for this. The high- and low-ionization zones of the BELR correspond to the cylindrical and conical regions of the wind, since the former is exposed to the full continuum while the latter receives only the continuum filtered by the former. The warm wind is significantly Thomson thick along the radial flow direction, producing the polarized optical continuum found in BALs, but is only partially ionized, creating a broad fluorescent 6.4 keV Fe-K emission line and greater than 10 keV Compton hump. The conical shell outflow can produce a biconical matter-bounded NELR. Luminosity-dependent changes in the structure, reducing the cylindrical part of the flow or increasing the mean angle to the disk axis and decreasing the wind opening angle, may explain the UV and X-ray Baldwin effects and the greater prevalence of obscuration in low-luminosity AGNs. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 138 TC 482 Z9 483 U1 2 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2000 VL 545 IS 1 BP 63 EP 76 DI 10.1086/317778 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 385RW UT WOS:000166018300007 ER PT J AU Wood, K Loeb, A AF Wood, K Loeb, A TI Escape of ionizing radiation from high-redshift galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : formation; HII regions; quasars : general ID HOPKINS-ULTRAVIOLET-TELESCOPE; ACTIVE GALACTIC NUCLEI; LY-ALPHA EMITTERS; COLD DARK MATTER; INTERSTELLAR-MEDIUM; CLUMPY MEDIA; COSMOLOGICAL REIONIZATION; MULTIPLE-SCATTERING; UNIVERSAL DENSITY; NEUTRAL HYDROGEN AB We use a three-dimensional radiation transfer code to calculate the steady state escape fraction of ionizing photons from disk galaxies as a function of redshift and galaxy mass. The gaseous disks are assumed to be isothermal (with a sound speed c(s) similar to 10 km s(-1)) and radially exponential. Their scale radius is related to the characteristic spin parameter and virial radius of their host halos, and their vertical structure is dictated by their self-gravity. The sources of radiation are taken to be either stars embedded in the disk or a central quasar. The predicted increase in the disk density with redshift results in an overall decline of the escape fraction with increasing redshift. For typical parameters of smooth disks, we find that the escape fraction at z similar to 10 is less than or similar to1% for stars but greater than or similar to 30% for miniquasars. Unless the smooth gas content of high-redshift disks was depleted by more than an order of magnitude due to supernovae-driven outflows or fragmentation, the reionization of the universe was most likely dominated by miniquasars rather than by stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wood, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kenny@claymore.harvard.edu; aloeb@cfa.harvard.edu NR 68 TC 91 Z9 91 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2000 VL 545 IS 1 BP 86 EP 99 DI 10.1086/317775 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 385RW UT WOS:000166018300009 ER PT J AU Bolatto, AD Jackson, JM Israel, FP Zhang, XL Kim, S AF Bolatto, AD Jackson, JM Israel, FP Zhang, XL Kim, S TI Carbon in the N159/N160 complex of the large Magellanic Cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : irregular; galaxies : ISM; ISM : clouds; Magellanic Clouds; radio lines : ISM; submillimeter ID SEST KEY PROGRAM; INFRARED EXTINCTION LAW; INTERSTELLAR CLOUDS; MOLECULAR CLOUDS; STAR-FORMATION; ATOMIC CARBON; DUST RATIO; GALAXIES; CO; GAS AB We present a study of carbon in N159/N160, an H II region complex in the low-metallicity Large Magellanic Cloud. We have mapped this region, which comprises four distinct molecular clouds spanning a wide range of star formation activity, in four transitions: (CO)-C-13 (J = 1 --> 0), (CO)-C-12 (J = 2 --> 1) and (J = 4 --> 3), and [C I] (P-3(1) --> P-3(0)). Combining these data with existing [C II] (P-2(3/2) --> P-2(1/2)) observations provides a complete picture of the predominant forms of carbon in the gas phase of the ISM. The new CO (J = 2 --> 1) data show that the complex is immersed in an envelope of extended, low-level emission, undetected by previous (J = 1 --> 0) mapping efforts. The (CO)-C-12 (J = 2 --> 1)/J = 1 --> 0) ratio in this envelope is greater than or similar to3, a value consistent with optically thin CO emission. The envelope is also relatively bright in [C I] and [C II], and calculations show that it is mostly photodissociated: it appears to be translucent (A(v) < 1). Neutral carbon emission in the complex unexpectedly peaks at the quiescent southern cloud (N159S). In the northern portion of the map (the N160 nebula), the H II regions prominent in [C II] correspond to holes in the [C I] distribution. Overall we find that, while the I-[CII]/I-CO ratio is enhanced with respect to similar complexes in the Milky Way, the I-[CI]/I-CO ratio appears to be similar or reduced. C1 Boston Univ, Dept Astron, Inst Astrophys Res, Boston, MA 02215 USA. Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Illinois, Dept Astron, Urbana, IL 61801 USA. RP Bolatto, AD (reprint author), Boston Univ, Dept Astron, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA. NR 49 TC 47 Z9 47 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2000 VL 545 IS 1 BP 234 EP 250 DI 10.1086/317794 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 385RW UT WOS:000166018300023 ER PT J AU Boroson, B O'Brien, K Horne, K Kallman, T Still, M Boyd, PT Quaintrell, H Vrtilek, SD AF Boroson, B O'Brien, K Horne, K Kallman, T Still, M Boyd, PT Quaintrell, H Vrtilek, SD TI Discovery of millihertz ultraviolet quasi-periodic oscillations in Hercules X-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; stars : individual (HZ Herculis); stars : oscillations; ultraviolet : stars; X-rays : stars ID TELESCOPE IMAGING SPECTROGRAPH; HZ HERCULIS; NEUTRON-STAR; 4U 1626-67; X-1; PULSAR; MASS; PULSATIONS; ACCRETION; SPECTRUM AB Observations of the ultraviolet continuum of the X-ray binary system Her X-1/HZ Herculis with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope (HST) show quasi-periodic oscillations (QPOs) at frequencies of 8 +/- 2 and 43 +/- 2 mHz, with rms amplitudes of 2% and 4% of the steady flux. Observations with the Keck Telescope confirm the presence of the higher frequency QPO in the optical continuum, with a rms amplitude of 1.6% +/- 0.2%. The QPOs are most prominent in the HST data near phi =0.5 (where phi =0 is the middle of the X-ray eclipse), suggesting that they arise not in the accretion disk but on the X-ray-heated face of the companion star. We discuss scenarios in which the companion star reprocesses oscillations in the disk which are caused by either Keplerian rotation or a beat frequency between the neutron star spin and Keplerian rotation at some radius in the accretion disk. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ St Andrews, St Andrews KY16 988, Fife, Scotland. Open Univ, Milton Keynes MK7 6AA, Bucks, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Boroson, B (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM bboroson@falafel.gsfc.nasa.gov; kso@st-andrews.ac.uk; kdh1@st-and.ac.uk; tim@xstar.gsfc.nasa.gov; still@chunky.gsfc.nasa.gov; padi@dragons.gsfc.nasa.gov; H.Quaintrell@open.ac.uk; svrtilek@cfa.harvard.edu RI Boyd, Patricia/D-3274-2012 NR 42 TC 16 Z9 16 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2000 VL 545 IS 1 BP 399 EP 406 DI 10.1086/317786 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 385RW UT WOS:000166018300038 ER PT J AU Baron, E Branch, D Hauschildt, PH Filippenko, AV Kirshner, RP Challis, PM Jha, S Chevalier, R Fransson, C Lundqvist, P Garnavich, P Leibundgut, B McCray, R Michael, E Panagia, N Phillips, MM Pun, CSJ Schmidt, B Sonneborn, G Suntzeff, NB Wang, L Wheeler, JC AF Baron, E Branch, D Hauschildt, PH Filippenko, AV Kirshner, RP Challis, PM Jha, S Chevalier, R Fransson, C Lundqvist, P Garnavich, P Leibundgut, B McCray, R Michael, E Panagia, N Phillips, MM Pun, CSJ Schmidt, B Sonneborn, G Suntzeff, NB Wang, L Wheeler, JC TI Preliminary spectral analysis of the Type II supernova 1999em SO ASTROPHYSICAL JOURNAL LA English DT Article DE radiative transfer; stars : atmospheres; supernovae : individual (SN 1999em) ID DISTANCE; ATMOSPHERES; SN-1993J; 1987A AB We have calculated fast direct spectral model fits to two early-time spectra of the Type II plateau SN 1999em, using the SYNOW synthetic spectrum code. The first is an extremely early blue optical spectrum and the second a combined Hubble Space Telescope and optical spectrum obtained one week later. Spectroscopically this supernova appears to be a normal Type II, and these fits are in excellent agreement with the observed spectra. Our direct analysis suggests the presence of enhanced nitrogen. We have further studied these spectra with the full non-LTE general model atmosphere code PHOENIX. While we do not find confirmation for enhanced nitrogen (nor do we rule it out), we do require enhanced helium. An even more intriguing possible line identification is complicated Balmer and He I lines, which we show falls naturally out of the detailed calculations with a shallow density gradient. We also show that very early spectra such as those presented here combined with sophisticated spectral modeling allow an independent estimate of the total reddening to the supernova, since when the spectrum is very blue, dereddening leads to changes in the blue flux that cannot be reproduced by altering the "temperature" of the emitted radiation. These results are extremely encouraging since they imply that detailed modeling of early spectra can shed light on both the abundances and total extinction of SNe II, the latter improving their utility and reliability as distance indicators. C1 Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Stockholm Observ, SE-13336 Saltsjobaden, Sweden. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. European So Observ, D-85748 Garching, Germany. Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Carnegie Inst Washington, Las Campanas Observ, La Serena, Chile. NASA, Goddard Space Flight Ctr, Astron & Solar Phys Lab, Greenbelt, MD 20771 USA. Australian Natl Univ, Mt Stromlo Observ, Weston, ACT 2611, Australia. NOAA, Cerro Tololo Interamer Observ, La Serena, Chile. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Baron, E (reprint author), Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. RI Baron, Edward/A-9041-2009; Sonneborn, George/D-5255-2012; OI Baron, Edward/0000-0001-5393-1608; Schmidt, Brian/0000-0001-6589-1287 NR 22 TC 92 Z9 93 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2000 VL 545 IS 1 BP 444 EP 448 DI 10.1086/317795 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 385RW UT WOS:000166018300043 ER PT J AU Barbera, M Micela, G Collura, A Murray, SS Zombeck, MV AF Barbera, M Micela, G Collura, A Murray, SS Zombeck, MV TI In-flight calibration of the ROSAT HRI ultraviolet sensitivity SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation : detectors; stars : early-type; stars : late-type; ultraviolet : stars; X-rays : stars ID STARS AB Comparing measured and estimated count rates of a few selected sample stars, we confirm the validity and provide the in-flight calibration of the ROSAT HRI UV/visible effective area model in Zombeck et al. The count rate estimates for Betelgeuse derived with this model are in agreement with the measured HRI upper limit. This result is also confirmed in an erratum by et al. aimed at revising their Berghofer previous calculation, which was overestimated by more than 2 orders of magnitude. Adopting this ROSAT HRI UV/visible effective area model and measured UV/visible spectra of a set of sample stars covering the range of T-eff 3000-40,000 K, we have built the calibration curves to estimate UV/visible contamination count rates for any star of known and T-eff, m(v), N-H. C1 Osservatorio Astron, Palermo, Italy. CNR, Ist Applicaz Interdisciplinari Fis, Palermo, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barbera, M (reprint author), Osservatorio Astron, GS Vaiana, Palermo, Italy. OI collura, alfonso/0000-0001-9534-1235; Barbera, Marco/0000-0002-3188-7420 NR 17 TC 5 Z9 5 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2000 VL 545 IS 1 BP 449 EP 453 DI 10.1086/317780 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 385RW UT WOS:000166018300044 ER PT J AU Lobel, A Dupree, AK AF Lobel, A Dupree, AK TI Modeling the variable chromosphere of alpha Orionis SO ASTROPHYSICAL JOURNAL LA English DT Article DE line : identification; stars : chromospheres; stars : individual (alpha Orionis); stars : late-type; stars : mass loss; supergiants ID HUBBLE-SPACE-TELESCOPE; LATE-TYPE STARS; CIRCUMSTELLAR ENVELOPES; EFFECTIVE TEMPERATURES; ULTRAVIOLET-SPECTRUM; OUTER ATMOSPHERES; GIANT STARS; II EMISSION; COOL STARS; BETELGEUSE AB A spectral analysis of the prototypical red supergiant star a Ori that is based on near-UV, optical, and near-IR high-dispersion spectra obtained between 1992 September and 1999 July with the Space Telescope Imaging Spectrograph and the Goddard High Resolution Spectrograph on the Hubble Space Telescope, the Utrecht Echelle Spectrograph, and the SoFin Echelle Spectrograph is presented. With detailed non-LTE radiative transfer calculations in spherical geometry, we model the mean conditions in the stellar chromosphere from H alpha and the Mg II resonance doublet. The H alpha absorption line emerges from an extended chromosphere. Temporal changes of its velocity structure are determined from detailed fits to near-UV Si I lines, and chromospheric expansion velocities around 4 km s(-1) are found in 1992, whereas the chromosphere was collapsing onto the photosphere with a velocity of 5 km s(-1) in 1998- 1999. The H alpha core depth is correlated over time with weaker depression changes seen in prominent TiO band heads that dominate the optical spectrum. From elaborate spectral synthesis calculations, we isolate unblended metal absorption lines in the near-IR and determine T-eff = 3500 K and log (g) = -0.5 for solar metallicity and 12 +/- 0.5 km s(-1) for macrobroadening and v sin i. Semiempirical fits yield chromospheric temperatures not in excess of 5500 K, but with long-term changes by similar to 400 K. The model extends over 5000 R-. and requires supersonic microturbulence values ranging to 19 km s(-1), in strong contrast with the photospheric value of only 2 km s(-1). We observe Doppler shifts of 4-8 km s(-1) in the scattering cores of many double-peaked near-UV emission lines which correlate with changes in the intensity ratio of their emission components. The red emission components were much stronger in 1992, indicating a phase of enhanced chromospheric outflow, for which we determine a spherical mass-loss rate of 6 x 10(-7) M-. yr(-1). We present a discussion of chromospheric pulsation in this massive star. Detailed modeling of the observed Mg II h and k line asymmetry is also presented. We demonstrate that a chromospheric Mn I blend strongly contributes to this puzzling asymmetry. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lobel, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 76 TC 36 Z9 36 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2000 VL 545 IS 1 BP 454 EP 474 DI 10.1086/317784 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 385RW UT WOS:000166018300045 ER PT J AU Gilliland, RL Brown, TM Guhathakurta, P Sarajedini, A Milone, EF Albrow, MD Baliber, NR Bruntt, H Burrows, A Charbonneau, D Choi, P Cochran, WD Edmonds, PD Frandsen, S Howell, JH Lin, DNC Marcy, GW Mayor, M Naef, D Sigurdsson, S Stagg, CR Vandenberg, DA Vogt, SS Williams, MD AF Gilliland, RL Brown, TM Guhathakurta, P Sarajedini, A Milone, EF Albrow, MD Baliber, NR Bruntt, H Burrows, A Charbonneau, D Choi, P Cochran, WD Edmonds, PD Frandsen, S Howell, JH Lin, DNC Marcy, GW Mayor, M Naef, D Sigurdsson, S Stagg, CR Vandenberg, DA Vogt, SS Williams, MD TI A lack of planets in 47 Tucanae from a Hubble Space Telescope search SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : eclipsing; globular clusters : individual (NGC 104, 47 Tucanae); planetary systems; techniques : photometric ID GLOBULAR-CLUSTERS; COMPANION AB We report results from a large Hubble Space Telescope project to observe a significant (similar to 34,000) ensemble of main-sequence stars in the globular cluster 47 Tucanae with a goal of defining the frequency of inner orbit, gas giant planets. Simulations based on the characteristics of the 8.3 days of time series data in the F555W and F814W Wide Field Planetary Camera 2 (WEPC2) filters show that similar to 17 planets should be detected by photometric transit signals if the frequency of hot Jupiters found in the solar neighborhood is assumed to hold for 47 Tuc. The experiment provided high-quality data sufficient to detect planets. A full analysis of these WFPC2 data reveals similar to 75 variables, but no light curves resulted for which a convincing interpretation as a planet could be made. The planet frequency in 47 Tuc is at least an order of magnitude below that for the solar neighborhood. The cause of the absence of close-in planets in 47 Tuc is not yet known; presumably the low metallicity and/or crowding of 47 Tuc interfered with planet formation; with orbital evolution to close-in positions, or with planet survival. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. Univ Texas, Dept Astron, Austin, TX 78712 USA. Aarhus Univ, Inst Phys & Astron, DK-8000 Aarhus, Denmark. Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Observ Geneva, CH-1290 Sauverny, Switzerland. Penn State Univ, Dept Astron, University Pk, PA 16802 USA. Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. RP Gilliland, RL (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. NR 21 TC 141 Z9 141 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2000 VL 545 IS 1 BP L47 EP L51 DI 10.1086/317334 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 388MP UT WOS:000166185100012 ER PT J AU Kastner, JH Soker, N Vrtilek, SD Dgani, R AF Kastner, JH Soker, N Vrtilek, SD Dgani, R TI Chandra X-ray observatory detection of extended X-ray emission from the planetary nebula BD+30 degrees 3639 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary nebulae : individual (BD+30 degrees 3639); stars : mass loss; stars : winds, outflows; X-rays : ISM ID CENTRAL STARS; ABELL-30; BUBBLE AB We report the detection of well-resolved, extended X-ray emission from the young planetary nebula BD + 30 degrees 3639 using the Advanced CCD Imaging Spectrometer (ACIS) aboard the Chandra X-ray Observatory. The X-ray emission from BD +30 degrees 3639 appears to lie within, but is concentrated to one side of, the interior of the shell of ionized gas seen in high-resolution optical and IR images. The relatively low X-ray temperature (T-x similar to 3 x10(6) K) and asymmetric morphology of the X-ray emission suggest that conduction fronts are present and/or mixing of shock-heated and photoionized gas has occurred, and furthermore hints at the presence of magnetic fields. The ACIS spectrum suggests that the X-ray-emitting region is enriched in the products of nuclear burning. Our detection of extended X-ray emission from BD +30 degrees 3639 demonstrates the power and utility of Chandra imaging as applied to the study of planetary nebulae. C1 Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. Univ Haifa Oranim, Dept Phys, IL-36006 Oranim, Tivon, Israel. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Kastner, JH (reprint author), Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA. NR 24 TC 59 Z9 59 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2000 VL 545 IS 1 BP L57 EP L59 DI 10.1086/317335 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 388MP UT WOS:000166185100014 ER PT J AU Waxman, E Loeb, A AF Waxman, E Loeb, A TI Fluctuations in the radio background from intergalactic synchrotron emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffuse radiation ID COMA-CLUSTER; RAY-EMISSION; UNIVERSE; GALAXIES AB The shocks produced in the intergalactic medium during large-scale structure formation accelerate a population of highly relativistic electrons that emit synchrotron radiation due to intergalactic magnetic fields. In a previous paper we have shown that these electrons cool primarily by inverse Compton scattering of the microwave background photons and can thereby produce the observed intensity and spectrum of the diffuse gamma -ray background. Here we calculate the intensity and angular fluctuations of the radio synchrotron background that results from the same high-energy electrons as well as the expected angular fluctuations in the gamma -ray background. On angular scales smaller than a degree, the predicted fluctuations in the microwave background temperature are of order 40 muK(xi (B)/0.01)(nu /10 GHz)(-3), where xi (B) is the magnetic fraction of the postshock energy density. This foreground might have already dominated the anisotropy signal detected in existing low-frequency cosmic microwave background experiments and can be identified with confidence through multifrequency observations. Detection of the synchrotron fluctuations would allow us to determine the strength of the intergalactic magnetic field. We predict a strong correlation between high-resolution maps taken at low-frequency radio waves and at high-energy gamma -rays. Young X-ray clusters may also appear as radio or gamma -ray clusters. The detailed study of this correlation will become easily accessible with the future launch of the Gamma-Ray Large-Area Space Telescope. C1 Weizmann Inst Sci, Dept Condensed Matter Phys, IL-76100 Rehovot, Israel. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Waxman, E (reprint author), Weizmann Inst Sci, Dept Condensed Matter Phys, POB 26, IL-76100 Rehovot, Israel. RI WAXMAN, ELI/K-1557-2012 NR 24 TC 41 Z9 41 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2000 VL 545 IS 1 BP L11 EP L14 DI 10.1086/317326 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 388MP UT WOS:000166185100003 ER PT J AU Geary, CM AF Geary, CM TI Photographing in the Cameroon Grassfields, 1970 to 1984 SO AFRICAN ARTS LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. RP Geary, CM (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 USA SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD WIN PY 2000 VL 33 IS 4 BP 70 EP + DI 10.2307/3337793 PG 0 WC Art SC Art GA 407RM UT WOS:000167284600010 ER PT J AU Pisano, DA AF Pisano, DA TI NASA and the space industry SO AMERICAN HISTORICAL REVIEW LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Pisano, DA (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU AMER HISTORICAL REVIEW PI WASHINGTON PA 400 A ST SE, WASHINGTON, DC 20003 USA SN 0002-8762 J9 AM HIST REV JI Am. Hist. Rev. PD DEC PY 2000 VL 105 IS 5 BP 1774 EP 1775 DI 10.2307/2652132 PG 2 WC History SC History GA 387NP UT WOS:000166128900108 ER PT J AU Arnoldi, MJ AF Arnoldi, MJ TI Africans on stage: Studies in ethnological show business SO AMERICAN HISTORICAL REVIEW LA English DT Book Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Arnoldi, MJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER HISTORICAL REVIEW PI WASHINGTON PA 400 A ST SE, WASHINGTON, DC 20003 USA SN 0002-8762 J9 AM HIST REV JI Am. Hist. Rev. PD DEC PY 2000 VL 105 IS 5 BP 1844 EP 1845 DI 10.2307/2652207 PG 2 WC History SC History GA 387NP UT WOS:000166128900186 ER PT J AU Allan, GJ Porter, JM AF Allan, GJ Porter, JM TI Tribal delimitation and phylogenetic relationships of Loteae and Coronilleae (Faboideae : Fabaceae) with special reference to Lotus: Evidence from nuclear ribosomal ITS sequences SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Coronilleae; Fabaceae; internal transcribed spacer; Loteae; Lotus; phylogeny ID TRANSCRIBED SPACER SEQUENCES; NUCLEOTIDE-SEQUENCES; POLLEN MORPHOLOGY; RBCL-SEQUENCES; LEGUMINOSAE; PAPILIONOIDEAE; DNA; GENE; EVOLUTION; TAXONOMY AB The temperate herbaceous tribes Loteae and Coronilleae have traditionally been regarded as taxonomically distinct entities. More recent morphological assessments, however, have challenged this view and suggest combining the two tribes under Loteae, Two key features used to distinguish the Coronilleae from Loteae include jointed fruits and branched root nodules. We evaluate the taxonomic utility of these characters using information derived from phylogenetic analyses of the internal transcribed spacers ITS1 + 2, and the intervening 5.8S region of nuclear ribosomal DNA. Results from this study show that neither the Loteae nor Coronilleae form individual monophyletic groups, and that key fruit and root nodule characters used to distinguish the Coronilleae are homoplastic. Given these data, we support the recognition of a single tribe, Loteae. We also find that Lotus, the largest and most morphologically complex genus in either tribe, is not monophyletic. Rather, it consists of two geographically distinct lineages, Old and New World, each of which are more closely related to other Loteae genera: Old World Lotus are more closely related to Old World Anthyllis, while New World Lotus show closer affinities to Old World Coronilla. These data also have important implications for the biogeography of New World Lotus: equally most parsimonious reconstructions suggest a complex scenario of intercontinental dispersals that involve not only Old World Lotus but Coronilla as well. C1 Rancho Santa Ana Bot Garden, Claremont, CA 91711 USA. RP Allan, GJ (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Lab Mol Systemat, Washington, DC 20560 USA. NR 70 TC 51 Z9 57 U1 1 U2 6 PU BOTANICAL SOC AMER INC PI COLUMBUS PA OHIO STATE UNIV-DEPT BOTANY, 1735 NEIL AVE, COLUMBUS, OH 43210 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD DEC PY 2000 VL 87 IS 12 BP 1871 EP 1881 DI 10.2307/2656839 PG 11 WC Plant Sciences SC Plant Sciences GA 384RE UT WOS:000165958000016 PM 11118424 ER PT J AU Brodie, RJ AF Brodie, RJ TI Ontogenetic changes in rates of water loss and shell-wearing behaviours enable land hermit crab megalopae to avoid desiccating in air. SO AMERICAN ZOOLOGIST LA English DT Meeting Abstract C1 Smithsonian Marine Stn, Ft Pierce, FL USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER SOC ZOOLOGISTS PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 0003-1569 J9 AM ZOOL JI Am. Zool. PD DEC PY 2000 VL 40 IS 6 BP 955 EP 955 PG 1 WC Zoology SC Zoology GA 422RA UT WOS:000168132000090 ER PT J AU Fauchald, K AF Fauchald, K TI Distribution of scales in polynoid scaleworms (Annelida, Polychaeta). SO AMERICAN ZOOLOGIST LA English DT Meeting Abstract C1 Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 1 Z9 1 U1 0 U2 1 PU AMER SOC ZOOLOGISTS PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 0003-1569 J9 AM ZOOL JI Am. Zool. PD DEC PY 2000 VL 40 IS 6 BP 1012 EP 1013 PG 2 WC Zoology SC Zoology GA 422RA UT WOS:000168132000234 ER PT J AU Henen, BT AF Henen, BT TI Reproductive effort and reproductive nutrition of female desert tortoises: essential field methods. SO AMERICAN ZOOLOGIST LA English DT Meeting Abstract C1 Univ Calif Los Angeles, Los Angeles, CA 90024 USA. Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ZOOLOGISTS PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 0003-1569 J9 AM ZOOL JI Am. Zool. PD DEC PY 2000 VL 40 IS 6 BP 1052 EP 1052 PG 1 WC Zoology SC Zoology GA 422RA UT WOS:000168132000333 ER PT J AU Maslakova, SA Martindale, MQ Norenburg, JL AF Maslakova, SA Martindale, MQ Norenburg, JL TI Remains of the pilidium in direct developing nemerteans? SO AMERICAN ZOOLOGIST LA English DT Meeting Abstract C1 George Washington Univ, Washington, DC 20052 USA. Kewalo Marine Lab, Honolulu, HI USA. Univ Hawaii, Honolulu, HI 96822 USA. Natl Museum Nat Hist, Washington, DC 20560 USA. Smithsonian Inst, Washington, DC 20560 USA. RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ZOOLOGISTS PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 0003-1569 J9 AM ZOOL JI Am. Zool. PD DEC PY 2000 VL 40 IS 6 BP 1119 EP 1119 PG 1 WC Zoology SC Zoology GA 422RA UT WOS:000168132000505 ER PT J AU Motz, AM Wolcott, TG Wolcott, DL Hines, AH AF Motz, AM Wolcott, TG Wolcott, DL Hines, AH TI Sperm limitation and operational sex ratio in blue crabs. SO AMERICAN ZOOLOGIST LA English DT Meeting Abstract C1 N Carolina State Univ, Raleigh, NC 27695 USA. Smithsonian Env Res Ctr, Edgewater, MD USA. NR 0 TC 0 Z9 0 U1 1 U2 2 PU AMER SOC ZOOLOGISTS PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 0003-1569 J9 AM ZOOL JI Am. Zool. PD DEC PY 2000 VL 40 IS 6 BP 1141 EP 1141 PG 1 WC Zoology SC Zoology GA 422RA UT WOS:000168132000559 ER PT J AU Norenburg, JL Roe, P AF Norenburg, JL Roe, P TI New sticky things in holopelagic nemerteans. SO AMERICAN ZOOLOGIST LA English DT Meeting Abstract C1 Smithsonian Inst, Washington, DC 20560 USA. Calif State Univ Stanislaus, Turlock, CA 95382 USA. RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ZOOLOGISTS PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 0003-1569 J9 AM ZOOL JI Am. Zool. PD DEC PY 2000 VL 40 IS 6 BP 1152 EP 1153 PG 2 WC Zoology SC Zoology GA 422RA UT WOS:000168132000587 ER PT J AU Pabst, DA Koopman, HN Rommel, SA Potter, CW Read, RJ McLellan, WA AF Pabst, DA Koopman, HN Rommel, SA Potter, CW Read, RJ McLellan, WA TI Ontogenetic allometry and body composition of harbor porpoises Phocoena phocoena from the Western North Atlantic. SO AMERICAN ZOOLOGIST LA English DT Meeting Abstract C1 Univ N Carolina, Wilmington, NC 28401 USA. Duke Univ, Durham, NC 27706 USA. Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 3 PU AMER SOC ZOOLOGISTS PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 0003-1569 J9 AM ZOOL JI Am. Zool. PD DEC PY 2000 VL 40 IS 6 BP 1159 EP 1159 PG 1 WC Zoology SC Zoology GA 422RA UT WOS:000168132000603 ER PT J AU Schwartz, ML Nor-Enburg, JL AF Schwartz, ML Nor-Enburg, JL TI Can we infer heteronemertean phylogeny from morphological data? SO AMERICAN ZOOLOGIST LA English DT Meeting Abstract C1 George Washington Univ, Washington, DC USA. Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ZOOLOGISTS PI LAWRENCE PA 1041 NEW HAMPSHIRE ST, LAWRENCE, KS 66044 USA SN 0003-1569 J9 AM ZOOL JI Am. Zool. PD DEC PY 2000 VL 40 IS 6 BP 1203 EP 1203 PG 1 WC Zoology SC Zoology GA 422RA UT WOS:000168132000713 ER PT J AU Paddayya, K Jhaldiyal, R Petraglia, MD AF Paddayya, K Jhaldiyal, R Petraglia, MD TI Excavation of an Acheulian workshop at Isampur, Karnataka (India) SO ANTIQUITY LA English DT Article C1 Deccan Coll, Dept Archaeol, Pune 411006, Maharashtra, India. Smithsonian Inst, Museum Natl Hist Nat, Dept Archaeol, Washington, DC 20560 USA. RP Paddayya, K (reprint author), Deccan Coll, Dept Archaeol, Pune 411006, Maharashtra, India. NR 3 TC 7 Z9 7 U1 0 U2 1 PU ANTIQUITY PUBL LTD PI CAMBRIDGE PA NEW HALL, CAMBRIDGE CB3 0DF, ENGLAND SN 0003-598X J9 ANTIQUITY JI Antiquity PD DEC PY 2000 VL 74 IS 286 BP 751 EP 752 PG 2 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 385NU UT WOS:000166011200010 ER PT J AU Winn, JN Hewitt, JN Schechter, PL Dressler, A Falco, EE Impey, CD Kochanek, CS Lehar, J Lovell, JEJ McLeod, BA Morgan, ND Munoz, JA Rix, HW Ruiz, MT AF Winn, JN Hewitt, JN Schechter, PL Dressler, A Falco, EE Impey, CD Kochanek, CS Lehar, J Lovell, JEJ McLeod, BA Morgan, ND Munoz, JA Rix, HW Ruiz, MT TI PMN J1838-3427: A new gravitationally lensed quasar SO ASTRONOMICAL JOURNAL LA English DT Article DE distance scale; gravitational lensing; quasars : individual (PMN J1838-3427) ID COSMOLOGICAL CONSTANT; SKY SURVEY; MODELS; MHZ AB We report the discovery of a new double-image quasar that was found during a search for gravitational lenses in the southern sky. Radio source PMN J1838-3427 is composed of two flat-spectrum components with separation 1."0, flux density ratio 14:1, and matching spectral indices in VLA and VLBA images. Ground-based BRI images show the optical counterpart (total I = 18.6) is also double, with the same separation and position angle as the radio components. An HST/WFPC2 image reveals the lens galaxy. The optical flux ratio (27: 1) is higher than the radio value, probably because of differential extinction of the components by the lens galaxy. An optical spectrum of the bright component contains quasar emission lines at z = 2.78 and several absorption features, including prominent Ly alpha absorption. The lens galaxy redshift could not be measured, but it is estimated to be z = 0.36 +/- 0.08. The image configuration is consistent with the simplest plausible models for the lens potential. The flat radio spectrum and observed variability of PMN J1838-3427 suggest that the time delay between flux variations of the components is measurable and could thus provide an independent measurement of H-o. C1 MIT, Dept Phys, Cambridge, MA 02139 USA. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. Inst Astrofis Canarias, E-38200 La Laguna, Tenerife, Spain. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Univ Chile, Dept Astron, Santiago, Chile. RP Winn, JN (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. RI Ruiz, Maria Teresa/I-5770-2016 OI Ruiz, Maria Teresa/0000-0002-6799-1537 NR 25 TC 31 Z9 31 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 SOUTH WOODLAWN AVE, CHICAGO, IL 60637-1603 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 2000 VL 120 IS 6 BP 2868 EP 2878 DI 10.1086/316874 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 383EU UT WOS:000165870800008 ER PT J AU Lada, CJ Muench, AA Haisch, KE Lada, EA Alves, JF Tollestrup, EV Willner, SP AF Lada, CJ Muench, AA Haisch, KE Lada, EA Alves, JF Tollestrup, EV Willner, SP TI Infrared L-band observations of the Trapezium cluster: A census of circumstellar disks and candidate protostars SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; infrared radiation; open clusters and associations : individual (Trapezium); stars : formation ID YOUNG STELLAR OBJECTS; ORION-NEBULA-CLUSTER; STAR-FORMATION; INTRINSIC COLORS; IMAGES; PHOTOMETRY; CLOUDS; DUST; CONDENSATIONS; RESOLUTION AB We report the results of a sensitive near-infrared JHKL imaging survey of the Trapezium cluster in Orion. We use the JHKL colors to obtain a census of infrared excess stars in the cluster. Of (391) stars brighter than 12th magnitude in the K and L bands, 80% +/- 7% are found to exhibit detectable infrared excess on the J-H, K-L color-color diagram. Examination of a subsample of 285 of these stars with published spectral types yields a slightly higher infrared excess fraction of 85%. We find that 97% of the optical proplyds in the cluster exhibit excess in the JHKL color-color diagram indicating that the most likely origin of the observed infrared excesses is from circumstellar disks. We interpret these results to indicate that the fraction of stars in the cluster with circumstellar disks is between 80%-85%, confirming earlier published suggestions of a high disk fraction for this young cluster. Moreover, we find that the probability of finding an infrared excess around a star is independent of stellar mass over essentially the entire range of the stellar mass function down to the hydrogen burning limit. Consequently, the vast majority of stars in the Trapezium cluster appear to have been born with circumstellar disks and the potential to subsequently form planetary systems, despite formation within the environment of a rich and dense stellar cluster. We identify 78 stars in our sample characterized by K-L colors suggestive of deeply embedded objects. The spatial distribution of these objects differs from that of the rest of the cluster members and is similar to that of the dense molecular cloud ridge behind the cluster. About half of these objects are detected in the short wavelength (J and H) bands, and these are found to be characterized by extreme infrared excess. This suggests that many of these sources could be protostellar in nature. If even a modest fraction (i.e., similar to 50%) of these objects are protostars, then star formation could be continuing in the molecular ridge at a rate comparable to that which produced the foreground Trapezium cluster. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. European So Observ, D-85748 Garching, Germany. RP Lada, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 52 TC 162 Z9 163 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 SOUTH WOODLAWN AVE, CHICAGO, IL 60637-1603 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 2000 VL 120 IS 6 BP 3162 EP 3176 DI 10.1086/316848 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 383EU UT WOS:000165870800028 ER PT J AU Torres, G Lacy, CHS Claret, A Sabby, JA AF Torres, G Lacy, CHS Claret, A Sabby, JA TI Absolute dimensions of the unevolved B-type eclipsing binary GG Orionis SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : eclipsing; binaries : spectroscopic; stars : evolution; stars : fundamental parameters; stars : individual (GG Orionis) ID MAIN-SEQUENCE; SPECTROSCOPIC BINARIES; STELLAR MODELS; EK-CEPHEI; STARS; CIRCULARIZATION; UBV; SYNCHRONIZATION; PHOTOMETRY; EVOLUTION AB We present photometric observations in B and V, as well as spectroscopic observations of the detached, eccentric 6.6 day double-lined eclipsing binary GG Ori, a member of the Orion OB1 association. Absolute dimensions of the components, which are virtually identical, are determined to high accuracy (better than 1% in the masses and better than 2% in the radii) for the purpose of testing various aspects of theoretical modeling. We obtain M-A = 2.342 +/- 0.016 M-. and R-A = 1.852 +/- 0.025 R-. for the primary, and M-B = 2.338 +/- 0.017 M-. and R-A = 1.830 +/- 0.025 R-. for the secondary. The effective temperature of both stars is 9950 +/- 200 K, corresponding to a spectral type of B9.5. GG Ori is very close to the zero-age main sequence, and comparison with current stellar evolution models gives ages of 65-82 Myr or 7.7 Myr, depending on whether the system is considered to be burning hydrogen on the main sequence or still in the final stages of pre-main-sequence contraction. Good agreement is found in both scenarios for a composition close to solar. We have detected apsidal motion in the binary at a rate of (omega) over dot = 0 degrees .00061 +/- 0 degrees .00025 cycle(-1), corresponding to an apsidal period of U = 10,700 +/- 4500 yr. A substantial fraction of this (similar to 70%) is due to the contribution from general relativity, and our measurement is entirely consistent with theory. The eccentric orbit of GG Ori is well explained by tidal evolution models, but both theory and our measurements of the rotational velocity of the components are as yet inconclusive as to whether the stars are synchronized with the orbital motion. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 76 TC 29 Z9 29 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 SOUTH WOODLAWN AVE, CHICAGO, IL 60637-1603 USA SN 0004-6256 J9 ASTRON J JI Astron. J. PD DEC PY 2000 VL 120 IS 6 BP 3226 EP 3243 DI 10.1086/316855 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 383EU UT WOS:000165870800033 ER PT J AU Trinchieri, G Pellegrini, S Wolter, A Fabbiano, G Fiore, F AF Trinchieri, G Pellegrini, S Wolter, A Fabbiano, G Fiore, F TI Broad band properties of medium and low L-x/L-b early type galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : individual : NGC 1407; galaxies : individual : NGC 1553; galaxies : individual : NGC 3115; galaxies : individual : NGC 3379; galaxies : individual : NGC 4125 ID X-RAY OBSERVATIONS; ELLIPTIC GALAXIES; ASTRONOMY SATELLITE; EMISSION MECHANISMS; ON-BOARD; HOT GAS; ASCA; SPECTRUM; M31 AB We have measured the spectral properties of five galaxies of low to intermediate L-x/L-b ratios with BeppoSAX and ASCA. A hard component (kT similar to 4 - 10 keV) is observed in all galaxies. In NGC 1553 the BeppoSAX data show that this component is extended, and suggest an origin for the emission in the evolved stellar population. In NGC 3115, a point-like source appears embedded in an extended component morphologically similar to the stellar body, suggesting an almost equal contribution from the nuclear region and the binary population. A large central mass concentration and low level optical activity in NGC 3379 argue for a contribution from the nucleus also in this object. However, for both NGC 3115 and NGC 3379, the nuclear emission is at a level well below that observed in other galaxies who host similar nuclear black holes. A second soft (kT similar to0.3- 0.7 keV) spectral component is needed to fit the data of NGC 1407, NGC 1553 and NGC 4125 over the entire energy range probed (similar to0.2-10 keV), best represented by a thermal component with line emission. We discuss possible interpretations of the origin of this component, which however will be better defined only with higher quality data. C1 Osserv Astron Brera, I-20121 Milan, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osservatorio Astron Roma, I-00044 Monteporzio Catone, Italy. RP Trinchieri, G (reprint author), Osserv Astron Brera, Via Brera 28, I-20121 Milan, Italy. EM ginevra@brera.mi.astro.it OI Wolter, Anna/0000-0001-5840-9835; Fiore, Fabrizio/0000-0002-4031-4157 NR 45 TC 9 Z9 9 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2000 VL 364 IS 1 BP 53 EP 69 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 392LJ UT WOS:000166412300017 ER PT J AU White, GJ Liseau, R Men'shchikov, AB Justtanont, K Nisini, B Benedettini, M Caux, E Ceccarelli, C Correia, JC Giannini, T Kaufman, M Lorenzetti, D Molinari, S Saraceno, P Smith, HA Spinoglio, L Tommasi, E AF White, GJ Liseau, R Men'shchikov, AB Justtanont, K Nisini, B Benedettini, M Caux, E Ceccarelli, C Correia, JC Giannini, T Kaufman, M Lorenzetti, D Molinari, S Saraceno, P Smith, HA Spinoglio, L Tommasi, E TI An infrared study of the L1551 star formation region SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : dust, extinction; ISM : individual objects :; L1551; ISM : jets and outflows; stars : pre-main sequence; infrared : ISM : lines and bands; infrared : stars ID LONG-WAVELENGTH SPECTROMETER; MOLECULAR CLOUDS; FE-II; TRANSITION-PROBABILITIES; COLLISION STRENGTHS; SUPERNOVA-REMNANTS; LINE EMISSION; IRON-PROJECT; SHOCK-WAVES; ATOMIC DATA AB Spectroscopic observations using the Infrared Space Observatory are reported towards the two well known infrared sources and young stellar objects L1551 IRS 5 and L1551 NE, and at a number of locations in the molecular outflow. The ISO spectrum contains several weak gas-phase lines of OI, CII, [Fe II] and [Si II], along with solid state absorption lines of CO, CO2, H2O, CH4 and CH3OH. Hubble Space Telescope (HST) images with the NICMOS infrared camera reveal a diffuse conical shaped nebulosity, due to scattered light from the central object, with a jet emanating from L1551 IRS 5. The continuum spectral energy distribution has been modelled using a 2D radiative transfer model, and fitted for a central source luminosity of 45 L., surrounding a dense torus extending to a distance of similar to 3 x 10(4) AU, which has a total mass of similar to 13 M.. The visual extinction along the outflow is estimated to be approximate to 10 and the mid-plane optical depth to L1551 IRS 5 to be approximate to 120. This model provides a good fit to the ISO spectral data, as well as to the spatial structures visible on archival HST/NICMOS data, mid-IR maps and sub-millimetre radio interferometry, and to ground-based photometry obtained with a range of different aperture sizes. On the basis of the above model, the extinction curve shows that emission at wavelengths shorter than similar to 2 mum is due to scattered light from close to L1551 IRS 5, while at wavelengths greater than or similar to 4 mum, is seen through the full extinguishing column towards the central source. Several [FeII] lines were detected in the SWS spectrum towards L1551 IRS 5. Although it would seem at first sight that shocks would be the most likely source of excitation for the [FeII] in a known shocked region such as this, the line intensities do not fit the predictions of simple shock models. An alternative explanation has been examined where the [Fe II] gas is excited in hot (similar to 4000 K) and dense (greater than or similar to 10(9) cm(-3)) material located close to the root of the outflow. The SWS observations did not detect any emission from rotationally excited Hz. Observations with United Kingdom Infrared Telescope (UKIRT) of the vibrationally excited S- and Q-branch lines were however consistent with the gas having an excitation temperature of similar to 2500 K. There was no evidence of lower temperature (similar to 500 K) H-2 gas which might be Visible in the rotational lines. Observations with UKIRT of the CO absorption bands close to 2.4 mum are best lit with gas temperatures similar to 2500 K, and a column density similar to 6 x 10(20) cm(-2) There is strong circumstantial evidence for the presence of dense (coronal and higher densities) and hot gas (at least 2500 K up to perhaps 5000 K) close to the protostar. However there is no obvious physical interpretation fitting all the data which can explain this. C1 Stockholm Observ, S-13336 Saltsjobaden, Sweden. Univ London Queen Mary & Westfield Coll, Dept Phys, London E1 4NS, England. Ist Fis Spazio Interplanetario, CNR, Area Ric Tor Vergata, I-00133 Rome, Italy. Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. CALTECH, IPAC, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Italian Space Agcy, I-00161 Rome, Italy. Univ La Sapienza, Ist Astron, I-00161 Rome, Italy. Cavendish Lab, Mullard Radio Astron Observ, Cambridge CB3 0HE, England. CESR, F-31028 Toulouse 4, France. RP White, GJ (reprint author), Stockholm Observ, S-13336 Saltsjobaden, Sweden. EM g.j.white@ukc.ac.uk RI Molinari, Sergio/O-4095-2016; OI Molinari, Sergio/0000-0002-9826-7525; Giannini, Teresa/0000-0002-0224-096X; /0000-0003-1689-9201; Spinoglio, Luigi/0000-0001-8840-1551; , Brunella Nisini/0000-0002-9190-0113 NR 85 TC 30 Z9 30 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2000 VL 364 IS 2 BP 741 EP 762 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 402PY UT WOS:000166998400050 ER PT J AU Gullbring, E Calvet, N Muzerolle, J Hartmann, L AF Gullbring, E Calvet, N Muzerolle, J Hartmann, L TI The structure and emission of the accretion shock in T Tauri stars. II. The ultraviolet-continuum emission SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; stars : formation; stars : pre-main-sequence; ultraviolet : stars ID BALMER LINE-PROFILES; BINARY GW-ORIONIS; MAGNETOSPHERIC ACCRETION; DISK ACCRETION; YOUNG STARS; EVOLUTION; MODELS AB We compare accretion-shock models with optical and ultraviolet spectra of pre-main-sequence stars to (1) make the first determinations of accretion rates in intermediate-mass T Tauri stars from continuum emission and (2) derive improved estimates of accretion rates and extinctions for continuum T Tauri stars. Our method extends the shock models developed by Calvet & Gullbring to enable comparisons with optical and archival International Ultraviolet Explorer ultraviolet spectra. We find good agreement between the observations and the model predictions, supporting the basic model of magnetospheric accretion shocks as well as previous determinations of accretion rates and interstellar reddening for the low-mass T Tauri stars. The accretion rates determined for the intermediate-mass T Tauri stars agree well with values obtained through the other methods of Muzerolle and coworkers that use near-infrared hydrogen line strengths. C1 Stockholm Observ, SE-13336 Saltsjobaden, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Ctr Invest Astron, Merida, Venezuela. Univ Massachusetts, Dept Astron, Five Coll, Lederle Grad Res Ctr 640, Amherst, MA 01003 USA. RP Gullbring, E (reprint author), Stockholm Observ, SE-13336 Saltsjobaden, Sweden. NR 28 TC 152 Z9 153 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2000 VL 544 IS 2 BP 927 EP 932 DI 10.1086/317253 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 384FA UT WOS:000165931100029 ER PT J AU Sobczak, GJ McClintock, JE Remillard, RA Cui, W Levine, AM Morgan, EH Orosz, JA Bailyn, CD AF Sobczak, GJ McClintock, JE Remillard, RA Cui, W Levine, AM Morgan, EH Orosz, JA Bailyn, CD TI Complete RXTE spectral observations of the black hole X-ray nova XTE J1550-564 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; stars : individual (XTE J1550-564); X-rays : stars ID MICROQUASAR GRO J1655-40; TIMING EXPLORER; PERFORMANCE; CANDIDATES AB We report on the X-ray spectral behavior of XTE J1550-564 during its 1998-1999 outburst. XTE J1550-564 is an exceptionally bright X-ray nova and is also the third Galactic black hole candidate known to exhibit quasi-periodic X-ray oscillations above 50 Hz. Our study is based on 209 pointed observations using the PCA and HEXTE instruments on board the Rossi X-Ray Timing Explorer (RXTE) spanning 250 days and covering the entire double-peaked eruption that occurred from 1998 September until 1999 May. The spectra are fitted to a model including multicolor blackbody disk and power-law components. The spectra from the first half of the outburst are dominated by the power-law component, whereas the spectra from the second half are dominated by the disk component. The source is observed in the very high and high/soft outburst states of black hole X-ray novae. During the very high state, when the power-law component dominated the spectrum, the inner disk radius is observed to vary by more than an order of magnitude; the radius decreased by a factor of 16 in one day during a 6.8 crab Rare. If the larger of these observed radii is taken to be the last stable orbit, then the smaller observed radius would imply that the inner edge of the disk is inside the event horizon! However, we conclude that the apparent variations of the inner disk radius observed during periods of increased power-law emission are probably caused by the failure of the multicolor disk/power-law model; the actual physical radius of the inner disk may remain fairly constant. This interpretation is supported by the fact that the observed inner disk radius remains approximately constant over 120 days in the high state, when the power-law component is weak, even though the disk flux and total flux vary by an order of magnitude. The mass of the black hole inferred by equating the approximately constant inner disk radius observed in the high/soft state with the last stable orbit for a Schwarzschild black hole is M-BH = 7.4 M.(D/6 kpc)(cos i)(-1/2). C1 Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Utrecht, Sterrekundig Inst, NL-3508 TA Utrecht, Netherlands. Yale Univ, Dept Astron, New Haven, CT 06520 USA. RP Sobczak, GJ (reprint author), Harvard Univ, Dept Astron, 60 Garden St,MS-10, Cambridge, MA 02138 USA. OI Cui, Wei/0000-0002-6324-5772 NR 32 TC 125 Z9 125 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2000 VL 544 IS 2 BP 993 EP 1015 DI 10.1086/317229 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 384FA UT WOS:000165931100035 ER PT J AU Luhman, KL AF Luhman, KL TI The initial mass function of low-mass stars and brown dwarfs in taurus SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : evolution; stars : formation; stars : low-mass, brown dwarfs; stars : luminosity function, mass function; stars : pre-main-sequence ID MAIN-SEQUENCE STARS; MOLECULAR CLOUDS; PLEIADES CLUSTER; FORMING REGIONS; YOUNG STARS; FIELD; SPECTROSCOPY; OPHIUCHUS; SPECTRUM; SEARCH AB By combining deep optical imaging and infrared spectroscopy with data from the Two-Micron All-Sky Survey (2MASS) and from previous studies (e.g., Briceno et al.), I have measured the initial mass function (IMF) for a reddening-limited sample in four fields in the Taurus star-forming region. This IMF is representative of the young populations within these fields for masses above 0.02 M.. Relative to the similarly derived IMF for the Trapezium Cluster (Luhman et al.), the IMF for Taurus exhibits a modest deficit of stars above 1 solar mass (i.e., steeper slope), the same turnover mass (similar to0.8 M.), and a significant deficit of brown dwarfs. If the IMF in Taurus were the same as that in the Trapezium, 12.8 +/- 1.8 brown dwarfs (>0.02 M.) are expected in these Taurus fields where only one brown dwarf candidate is found. These results are used to test theories of the IMF. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 53 TC 115 Z9 115 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2000 VL 544 IS 2 BP 1044 EP 1055 DI 10.1086/317232 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 384FA UT WOS:000165931100038 ER PT J AU Coil, AL Matheson, T Filippenko, AV Leonard, DC Tonry, J Riess, AG Challis, P Clocchiatti, A Garnavich, PM Hogan, CJ Jha, S Kirshner, RP Leibundgut, B Phillips, MM Schmidt, BP Schommer, RA Smith, RC Soderberg, AM Spyromilio, J Stubbs, C Suntzeff, NB Woudt, P AF Coil, AL Matheson, T Filippenko, AV Leonard, DC Tonry, J Riess, AG Challis, P Clocchiatti, A Garnavich, PM Hogan, CJ Jha, S Kirshner, RP Leibundgut, B Phillips, MM Schmidt, BP Schommer, RA Smith, RC Soderberg, AM Spyromilio, J Stubbs, C Suntzeff, NB Woudt, P TI Optical spectra of Type Ia supernovae at z=0.46 and z=1.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; supernovae : general; supernovae : individual (SN 1999ff, SN 1999fv) ID UNIVERSE; EVOLUTION; AGE AB We present optical spectra, obtained with the Keck 10 m telescope, of two high-redshift Type Ia supernovae (SNe Ia) discovered by the High-z Supernova Search Team: SN 1999ff at z = 0.455 and SN 1999fv at z similar to 1.2, the highest redshift published SN Ia spectrum. Both SNe were at maximum light when the spectra were taken. We compare our high-z spectra with low-z normal and peculiar SNe Ia as well as with SNe Ic, Ib, and II. There are no significant differences between SN 1999ff and normal SNe Ia at low redshift. SN 1999fv appears to be an SN Ia and does not resemble the most peculiar nearby SNe Ia. C1 Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Hawaii, Astron Inst, Honolulu, HI 96822 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. European So Observ, D-85748 Garching, Germany. Univ Washington, Dept Astron, Seattle, WA 98195 USA. European So Observ, D-85748 Garching, Germany. Cerro Tololo Interamer Observ, La Serena, Chile. Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Coil, AL (reprint author), Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Schmidt, Brian/0000-0002-8538-9195 NR 32 TC 44 Z9 44 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2000 VL 544 IS 2 BP L111 EP L114 DI 10.1086/317311 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 384FC UT WOS:000165931300007 ER PT J AU Hatzes, AP Cochran, WD McArthur, B Baliunas, SL Walker, GAH Campbell, B Irwin, AW Yang, S Kurster, M Endl, M Els, S Butler, RP Marcy, GW AF Hatzes, AP Cochran, WD McArthur, B Baliunas, SL Walker, GAH Campbell, B Irwin, AW Yang, S Kurster, M Endl, M Els, S Butler, RP Marcy, GW TI Evidence for a long-period planet orbiting epsilon Eridani SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars : individual (epsilon Eridani); stars : low-mass, brown dwarfs; techniques : radial velocities ID TIME-SERIES; STARS; BINARY; ECCENTRICITY; SPECTROMETER; 16-CYGNI-B; ASTROMETRY; COMPANIONS; TELESCOPE; SEARCH AB High-precision radial velocity (RV) measurements spanning the years 1980.8-2000.0 are presented for the nearby (3.22 pc) K2 V star epsilon Eri. These data, which represent a combination of six independent data sets taken with four different telescopes, show convincing variations with a period of approximate to7 yr. A least-squares orbital solution using robust estimation yields orbital parameters of period P = 6.9 yr, velocity amplitude K = 19 m s(-1), eccentricity e = 0.6, projected companion mass M sin i = 0.86 M-Jupiter and semimajor axis a(2) = 3.4 AU. Ca II H and K S-index measurements spanning the same time interval show significant variations with periods of 3 and 20 yr yet none at the RV period. If magnetic activity were responsible for the RV variations, then it produces a significantly different period than is seen in the Ca II data. Given the lack of Ca II variation with the same period as that found in the RV measurements, the long-lived and coherent nature of these variations, and the high eccentricity of the implied orbit, Keplerian motion due to a planetary companion seems to be the most likely explanation for the observed RV variations. The wide angular separation of the planet from the star (approximately 1 ") and the long orbital period make this planet a prime candidate for both direct imaging and space-based astrometric measurements. C1 Univ Texas, McDonald Observ, Austin, TX 78712 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ British Columbia, Dept Phys & Astrophys, Vancouver, BC V6T 1Z4, Canada. Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. European So Observ, Santiago 19, Chile. Agr Univ Vienna, Inst Astron, A-1180 Vienna, Austria. Univ Heidelberg, Inst Theoret Astrophys, D-69121 Heidelberg, Germany. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Hatzes, AP (reprint author), Univ Texas, McDonald Observ, Austin, TX 78712 USA. RI Butler, Robert/B-1125-2009 NR 33 TC 138 Z9 138 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2000 VL 544 IS 2 BP L145 EP L148 DI 10.1086/317319 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 384FC UT WOS:000165931300015 ER PT J AU Bosch, J Rand, AS Ryan, MJ AF Bosch, J Rand, AS Ryan, MJ TI Signal variation and call preferences for whine frequency in the tungara frog, Physalaemus pustulosus SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE signal variation; call preferences; tungara frog ID TOADS ALYTES OBSTETRICANS; FEMALE MATE CHOICE; NEOTROPICAL FROG; SEXUAL SELECTION; SENSORY EXPLOITATION; CISTERNASII; EVOLUTION AB Properties of sexual signals can differ in the amount of within-male variability. In several species of anurans, females exert stabilizing or weakly directional preferences on less variable call properties, and highly directional preferences on more variable ones. Preferences of female tungara frogs, Physalaemus pustulosus, were examined for two call characteristics: a less variable spectral character, dominant frequency of the whine, and a more variable temporal character, inter-call interval. Eight phonotaxis experiments using synthetic calls were conducted with gravid females. Stimuli presented for both characters were based on the mean and standard deviation (SD) of those characters in the study population. For each character, we used four intervals of variation (1, 2, 3, and 4 SD) between stimuli in four different experiments. As has been found in some other anuran species, preference was stronger for the more variable temporal character, increasing in proportion to the difference between stimuli. Preference for the less variable spectral character was not significant until the difference between stimuli was substantial. The strength of female preference, estimated as latency to choose, the number of speakers visited, and the number of females showing phonotaxis, increased in proportion to the increase in the difference between stimuli. All these measures of strength of preference were greater in response to the more variable temporal character compared to responses to the less variable spectral character. C1 CSIC, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain. Smithsonian Trop Res Inst, Balboa, Panama. Univ Texas, Sect Integrat Biol C0930, Austin, TX 78712 USA. RP Bosch, J (reprint author), CSIC, Museo Nacl Ciencias Nat, Jose Gutierrez Abascal 2, E-28006 Madrid, Spain. RI Bosch, Jaime/H-3042-2011; OI Bosch, Jaime/0000-0002-0099-7934 NR 19 TC 30 Z9 30 U1 0 U2 6 PU SPRINGER-VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD DEC PY 2000 VL 49 IS 1 BP 62 EP 66 DI 10.1007/s002650000280 PG 5 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 387ZE UT WOS:000166152300009 ER PT J AU Stephens, C Dennis, M AF Stephens, C Dennis, M TI Engineering time: inventing the electronic wristwatch SO BRITISH JOURNAL FOR THE HISTORY OF SCIENCE LA English DT Article AB In the late 1960s teams of engineers working independently in Japan, Switzerland and the United States used newly created electronic components to completely reinvent the wristwatch. The products these groups developed instigated a global revolution in the watch industry and gave everyone, whether they needed it or not, access to the split-second accuracy once available only to scientists and technicians. This radical change in timekeeping technology was in the vanguard of a dramatic shift from a mechanical to an electronic world and raises important issues about technological change for scholars interested in late twentieth-century history. Examining the work of three teams of engineers, this paper offers a comparative approach to understanding how local differences in culture, economy, business structure and access to technological knowledge shaped the design of finished products and their acceptance by users. C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Stephens, C (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 70 TC 4 Z9 4 U1 0 U2 4 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH STREET, NEW YORK, NY 10011-4211 USA SN 0007-0874 J9 BRIT J HIST SCI JI Br. J. Hist. Sci. PD DEC PY 2000 VL 33 IS 119 BP 477 EP 497 DI 10.1017/S0007087400004167 PN 4 PG 21 WC History & Philosophy Of Science SC History & Philosophy of Science GA 402NH UT WOS:000166994700006 ER PT J AU Safronova, UI Vasilyev, AA Smith, RK AF Safronova, UI Vasilyev, AA Smith, RK TI Satellite dielectronic spectra created from autoionizing 2lnl ' and 1s2lnl ' states with n=4-5 SO CANADIAN JOURNAL OF PHYSICS LA English DT Article ID LI-LIKE IONS; ENERGY-LEVELS; Z-DEPENDENCES; HE-LIKE; RATES; SYSTEMS; LINES AB The relative intensities of dielectronic satellite lines determined by radiative transition probabilities and autoionization rates are calculated for the transitions 2lnl' - 1snl'', 2lnl' - 1s2l (n = 4-5, l' = 0-3, l'' = 0-3, l = 0-1) in He-like ions and for the transitions 1s2lnl' - 1s(2)nl'', 1s2lnl' - 1s(2)2l (n = 4-5, l' =0-3, l'' = 0-3, l = 0-1) in Li-like ions, for all Z = 5-54, using the perturbation theory method (Z-expansion). Relativistic effects are taken into account using the Breit-Pauli operators. The asymptotic dependence on n of the energy matrix is discussed for 2lnl' and 1s2lnl' autoionizing states. The intermediate coupling coefficients obtained after diagonalization of the energy matrices are also studied. It was observed that these coefficients change very sharply with n and Z due to a redistribution of the contributions of relativistic and correlation effects. As a result, all other atomic characteristics (radiative and nonradiative transition rates, branching ratios, and relative intensity factor) display nonmonotonic Z- and n-dependencies with maxima and minima. C1 Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Safronova, UI (reprint author), Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. NR 18 TC 9 Z9 9 U1 0 U2 1 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA SN 0008-4204 J9 CAN J PHYS JI Can. J. Phys. PD DEC PY 2000 VL 78 IS 12 BP 1055 EP 1067 DI 10.1139/cjp-78-12-1055 PG 13 WC Physics, Multidisciplinary SC Physics GA 418RU UT WOS:000167905800002 ER PT J AU Kleiman, DG Reading, RP Wallace, RL Robinson, J Cabin, RJ Felleman, F AF Kleiman, DG Reading, RP Wallace, RL Robinson, J Cabin, RJ Felleman, F TI Improving the value of conservation programs SO CONSERVATION BIOLOGY LA English DT Letter C1 Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. Denver Zool Fdn, Denver, CO 80218 USA. Eckerd Coll, St Petersburg, FL 33701 USA. Wildlife Conservat Soc, Bronx, NY 10460 USA. USDA, Forest Serv, Hilo, HI 96720 USA. Conservat Consultants Inc, Seattle, WA 98117 USA. RP Kleiman, DG (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA. NR 0 TC 1 Z9 1 U1 0 U2 4 PU BLACKWELL SCIENCE INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD DEC PY 2000 VL 14 IS 6 BP 1569 EP 1569 DI 10.1046/j.1523-1739.2000.01462-2.x PG 1 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 385ZV UT WOS:000166035800003 ER PT J AU Bruno, MC Reid, JW Perry, SA AF Bruno, MC Reid, JW Perry, SA TI New records of copepods from Everglades National Park (Florida): description of two new species of Elaphoidella (Harpacticoida, Canthocamptidae), and supplementary description of Diacyclops nearcticus Kiefer (Cyclopoida, Cyclopidae) SO CRUSTACEANA LA English DT Article ID UNITED-STATES; CRUSTACEA; USA AB Two new species of harpacticoid copepods from Everglades National Park Florida, Elaphoidella marjolyae sp. nov. and Elaphoidella fluviusherbae sp. nov., are described. Whereas E. majoryae was collected from both surface waters and groundwater, E. fluviusherbae was found only in groundwater. The new species differ from congeners mainly in details of setation and spination of the swimming legs, and the shape and setation of the caudal rami. The ecology and geographical distribution of the genus Elaphoidella in North America are presented and discussed. The find of the cyclopoid copepod Diacyclops nearcticus Kiefer in the Eveglades extends the known distribution of this North American species considerably southward. We present supplementary observations on the morphology of the female, including some obtained by scanning electron microscopy, and we describe the male. Geographical distribution and known habitats of the species are also presented and discussed. C1 Everglades Natl Pk, S Florida Nat Resources Ctr, Homestead, FL 33034 USA. Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Bruno, MC (reprint author), Everglades Natl Pk, S Florida Nat Resources Ctr, Homestead, FL 33034 USA. RI Bruno, Maria Cristina/D-8792-2011; Bruno, Maria Cristina/B-8117-2015 OI Bruno, Maria Cristina/0000-0001-7860-841X; Bruno, Maria Cristina/0000-0001-7860-841X NR 29 TC 9 Z9 9 U1 0 U2 5 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X J9 CRUSTACEANA JI Crustaceana PD DEC PY 2000 VL 73 BP 1171 EP 1204 DI 10.1163/156854000505164 PN 10 PG 34 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 405FC UT WOS:000167146600001 ER PT J AU Herken, G AF Herken, G TI In the service of the state: Science and the Cold War SO DIPLOMATIC HISTORY LA English DT Article C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Herken, G (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 28 TC 2 Z9 2 U1 0 U2 0 PU BLACKWELL PUBLISHERS PI MALDEN PA 350 MAIN STREET, STE 6, MALDEN, MA 02148 USA SN 0145-2096 J9 DIPLOMATIC HIST JI Dipl. Hist. PD WIN PY 2000 VL 24 IS 1 BP 107 EP 115 DI 10.1111/0145-2096.00200 PG 9 WC History SC History GA 290NK UT WOS:000085682100005 ER PT J AU Adey, WH AF Adey, WH TI Coral reef ecosystems and human health: Biodiversity counts! SO ECOSYSTEM HEALTH LA English DT Article ID CALCIFICATION; CARBONATE; PHOTOSYNTHESIS; COMMUNITY; CALCIUM; OCEAN AB The health of human populations requires a wide variety of chemical and physical supports from their associated ecosystems, as well as from the global ecosystem. Ecosystems can be "ecologically engineered" to improve the efficiency of that service, particularly when ecosystem health fails due to human overloads. Less well recognized is an entirely different dimension of ecosystem support of human populations; namely the pharmacological value of ecosystem biodiversity. Natural product chemistries are an extremely important resource in the ever-expanding human battle with health degrading microbes. Coral reefs are the most diverse ecosystems in the sea and have the highest density of biodiversity globally. High diversity density gives rise to intense species competition and the subsequent organism capability to construct exotic defensive and offensive chemicals, many with pharmacological value. Coral reefs are being rapidly degraded, anthropogenically, both locally and globally. It is estimated that less than 10% of reef biodiversity is currently known and only a small fraction of that percent has been tested for "active compounds". Many species extinctions are likely in the coming decades, and badly needed pharmacological potential will subsequently be lost. Sophisticated coral reef and reef organism culturing capability is now available that would allow the prospecting of reefs, the efficient analysis of organisms and eventually the mass culturing of those organisms for their secondary compounds without ecosystem damage. The economic value of this pharmaceutical potential needs to be directed by governments to an international crash project to conserve coral reefs and their biodiversity. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Adey, WH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. NR 52 TC 5 Z9 7 U1 2 U2 13 PU BLACKWELL SCIENCE INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 1076-2825 J9 ECOSYST HEALTH JI Ecosyst. Health PD DEC PY 2000 VL 6 IS 4 BP 227 EP 236 DI 10.1046/j.1526-0992.2000.006004227.x PG 10 WC Ecology; Environmental Studies SC Environmental Sciences & Ecology GA 410EG UT WOS:000167426600003 ER PT J AU Winter, K Garcia, M Lovelock, CE Gottsberger, R Popp, M AF Winter, K Garcia, M Lovelock, CE Gottsberger, R Popp, M TI Responses of model communities of two tropical tree species to elevated atmospheric CO2: growth on unfertilized soil SO FLORA LA English DT Article DE CO2 exchange; elevated CO2; growth; trees; tropical forest ID ECOSYSTEMS; SEEDLINGS; FORESTS; PLANTS AB Biomass accumulation of model seedling communities of two tropical tree species was studied at ambient and elevated CO2 levels (four replicates per CO2 concentration), using open-top chambers situated in a cleared area at the edge of a tropical forest near Panama City, Republic of Panama. Each chamber (diameter about 2 m) contained a mixture of 18 plants of Ficus insipida, a fast-growing pioneer species, and 18 plants of Virola surinamensis, a slow-growing late-successional species. Plants grew in well-drained, well-watered, loose, unfertilized soil. During the 30 week experimental period, biomass accumulation by F. insipida, which increased in height from about 20 to 180 cm, predominated, whereas V. surinamensis grew only slowly in the strongly shaded understorey. Neither community biomass accumulation (above- plus belowground) nor the biomass ratio (F. insipida: V. surinamensis) of the two species was significantly affected by elevated CO2, although community biomass accumulation was on average slightly higher at elevated than at ambient CO2, and the biomass of F: insipida increased on average relative to V. surinamensis at elevated CO2. Plants grown at elevated CO2 contained greater levels of starch and lower levels of nitrogen per unit leaf dry mass, and, therefore, showed higher ratios of C:N than plants at ambient CO2. Specific leaf area, the area per unit leaf dry mass; and the leaf area ratio (LAR), the total leaf area per total plant dry mass, decreased in response to elevated CO2. This decrease in LAR counteracted the potential effect on biomass gain of increases in both net assimilation rate (the rate of dry mass accumulation per unit leaf area) and rates of photosynthetic leaf net CO2 uptake at elevated as compared to ambient CO2, particularly in Ficus insipida. C1 Smithsonian Trop Res Inst, Balboa, Panama. Univ Vienna, Inst Pflanzenphysiol, A-1091 Vienna, Austria. RP Winter, K (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama. RI Popp, Marianne/E-7559-2012; Lovelock, Catherine/G-7370-2012 OI Lovelock, Catherine/0000-0002-2219-6855 NR 22 TC 23 Z9 24 U1 1 U2 9 PU URBAN & FISCHER VERLAG PI JENA PA BRANCH OFFICE JENA, P O BOX 100537, D-07705 JENA, GERMANY SN 0367-2530 J9 FLORA JI Flora PD DEC PY 2000 VL 195 IS 4 BP 289 EP 302 PG 14 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 390AY UT WOS:000166272500001 ER PT J AU McLaughlin, PA Lemaitre, R AF McLaughlin, PA Lemaitre, R TI Aspects of evolution in the anomuran superfamily Paguroidea: one larval prospective SO INVERTEBRATE REPRODUCTION & DEVELOPMENT LA English DT Article; Proceedings Paper CT 2nd Crustacean Larval Conference CY SEP 06-09, 1999 CL LISBON, PORTUGAL DE larval development; carcinization; abdominal evolution; Anomura; Paguroidea; Lithodidae ID EARLY JUVENILE DEVELOPMENT; LITHODIDAE DECAPODA; HERMIT-CRAB; CARCINIZATION AB McLaughlin and Lemaitre (1997), in their examination of carcinization in the Anomura, rejected the traditional concept of paguroid evolution, which had consistently maintained that the lithodid crab-like body form evolved from a typical shell-dwelling hermit crab. Their hypothesis proposed just the reverse, i.e., the lithodid crab-like body form gave rise to the simple hermit crab body form through calcium loss, habitat change and consequential morphological adaptations. Their original hypothesis was based on characters derived from adult morphology, but they suggested that larval data would support their view. The megalopal and first or first- and second-crab stages of representatives of both subfamilies of the Lithodidae provide the first of such larval information. Ten species in eight genera have been examined specifically for development of abdominal tergites. These data, although preliminary in scope, unequivocally disprove the Bouvierian concept of lithodid abdominal plate development, and in so doing, lend substantial support to McLaughlin and Lemaitre's hypothesis. C1 Western Washington Univ, Shannon Point Marine Ctr, Anacortes, WA 98221 USA. Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP McLaughlin, PA (reprint author), Western Washington Univ, Shannon Point Marine Ctr, 1900 Shannon Point Rd, Anacortes, WA 98221 USA. NR 32 TC 10 Z9 10 U1 1 U2 2 PU INT SCIENCE SERVICES/BALABAN PUBLISHERS PI REHOVOT PA PO BOX 2039, REHOVOT 76120, ISRAEL SN 0168-8170 J9 INVERTEBR REPROD DEV JI Invertebr. Reprod. Dev. PD DEC PY 2000 VL 38 IS 3 BP 159 EP 169 DI 10.1080/07924259.2000.9652453 PG 11 WC Reproductive Biology; Zoology SC Reproductive Biology; Zoology GA 406HB UT WOS:000167207900002 ER PT J AU Moyer, AE AF Moyer, AE TI The papers of Joseph Henry, vol 7: January 1847-December 1849: The Smithsonian years. SO ISIS LA English DT Book Review C1 Virginia Tech, Dept Hist, Blacksburg, VA USA. Smithsonian Inst, Washington, DC 20560 USA. RP Moyer, AE (reprint author), Virginia Tech, Dept Hist, Blacksburg, VA USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD DEC PY 2000 VL 91 IS 4 BP 794 EP 795 DI 10.1086/384985 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 414HX UT WOS:000167661700042 ER EF